44 Validated Planets from K2 Campaign 10

In C10, K2 observed a ∼110 square degree field near the North Galactic cap from 2016 July 06 to 2016 September 20. Long-cadence (30 minute) exposures of 28345 target stars were downlinked from the spacecraft, and the data were calibrated and subsequently made available on the Mikulski Archive for Space Telescopes²³ (MAST). During the beginning of the campaign, a 3.5-pixel pointing error was detected and subsequently corrected six days after the start of observations. The data during this time is of substantially lower quality than the rest of the campaign, so we discard it in our analysis. An additional data gap was the result of the failure of detector module 4, which caused the photometer to power off for 14 days.

Following the loss of two of its four reaction wheels, the Kepler spacecraft has been operating as K2 (Howell et al. 2014). The dominant systematic signal in K2 light curves is caused by the rolling motion of the spacecraft along its bore sight coupled with inter- and intra-pixel sensitivity variations. We used a method similar to that described by Vanderburg & Johnson (2014) to reduce this systematic flux variation. Our light curve production pipeline is as follows. We first downloaded the target pixel files from MAST. We laid circular apertures around the brightest pixel within the "postage stamp" (the set of pixels of the Kepler photometer corresponding to a given source). To obtain the centroid position of the image, we fitted a two-dimensional (2D) Gaussian function to the in-aperture flux distribution. We then fitted a piecewise linear function between the flux variation and the centroid motion of target. The fitted piecewise linear function was then detrended from the observed flux variation.

Before searching the light curve for transits, we first removed any long-term systematic or instrumental flux variations by fitting a cubic spline to the reduced light curve from the previous section. To look for periodic transit signals, we employed the box-least-squares algorithm (BLS; Kovács et al. 2002). We improved the efficiency of the original BLS algorithm by using a nonlinear frequency grid that takes into account the scaling of transit duration with orbital period (Ofir 2014). We also adopted the signal detection efficiency (SDE; Ofir 2014), which quantifies the significance of a detection. SDE is defined by the amplitude of peak in the BLS spectrum normalized by the local standard deviation. We empirically set a threshold of SDE > 6.5 for the balance between completeness and false alarm rate. In order to identify all the transiting planets in the same system, we progressively re-ran BLS after removing the transit signal detected in the previous iteration.

To search for additional transit signals that may have been missed by the transit search method described above, we used two separate pipelines: one based on the DST code (Cabrera et al. 2012), and one based on the wavelet-based filter routines VARLET and PHALET (Grziwa & Pätzold 2016). This helps to ensure higher detection rates, and the number of false positives is potentially reduced by utilizing multiple diagnostics. The DST code is optimized for space-based photometry and has been successfully applied to data from CoRoT and Kepler; we ran it on the light curves extracted by Vanderburg & Johnson (2014), which are publicly available from MAST. In the wavelet-based search, we first used VARLET to remove long-term stellar variability in the light curves and then searched for transits using a modified version of the BLS algorithm. Detected transit-like signals were then removed using PHALET, which combines phase-folding and a wavelet basis to approximate periodic features. In similar fashion to the above approach, we iterate this process of feature detection and removal to enable the detection of multi-planet systems.

We performed a quick initial vetting to identify obvious false positives among the transiting signals identified in the previous section. Planetary candidates that survived the various tests were followed up with speckle imaging and reconnaissance spectra for proper statistical validation. We tested for the presence of any "odd–even" variations and significant secondary eclipse, both of which are likely signatures of eclipsing binaries. The odd–even effect is the variation of the eclipse depth between the primary and secondary eclipse of an eclipsing binary. If mistaken for planetary transits, the primary and secondary eclipses will be the odd and even numbered transits.

We fitted Mandel & Agol (2002) model to the odd and even transits separately. If a system shows odd–even variations with more than 3σ significance, it is flagged as a false positive. We also looked for any secondary eclipse in the light curve, using the Mandel & Agol (2002) model fit of the transits as a template for the occultation. After fitting the primary transits, we searched for secondary eclipses via an additional MCMC fitting step. We set the limb-darkening coefficients to zero and fixed all transit parameters except for two: the time of secondary eclipse and the depth of the eclipse. The resulting posterior distributions of these two parameters were then used to quantify the significance and phase of any putative secondary eclipses. For non-detections, we use the 3σ upper limit derived from the eclipse depth posterior to set the "maximum allowed secondary eclipse" constraint in our vespa analyses. If a system shows a secondary eclipse with more than 3σ significance, we calculated the geometric albedo using the depth of secondary eclipse. The object is likely self-luminous, hence likely a false positive, if the albedo is much greater than 1.

We also measured stellar rotation periods P_rot from the variability in the light curves induced by starspot modulation. About half of the light curves of our candidates exhibited a lack of rotational modulation, or the K2 C10 time baseline was not long enough to constrain the period. For the rest, we used the autocorrelation function (ACF; e.g., McQuillan et al. 2014) to measure the rotational period, and we include these results in Table 1 along with initial estimates of the basic transit parameters of each candidate. To help ensure the validity of these measurements, we also used the Lomb–Scargle periodogram (Lomb 1976; Scargle 1982) to measure the rotational periods, and the results were in good agreement.

Table 1.  Candidate Planets Detected in K2 C10

EPIC	Kp	Porb	T0	T14	Depth	SDE	Prot
	(mag)	(days)	(BKJD)	(hr)			(days)
201092629	11.9	26.810	2751.22	4.1	0.00090	13.2	${22}_{-2}^{+6}$
201102594	15.6	6.514	2753.24	2.0	0.00624	8.2	25 ± 3
201110617	12.9	0.813	2750.14	1.3	0.00029	16.2	16.8 ± 2.5
201111557	11.4	2.302	2750.17	1.9	0.02268	7.6	12.0 ± 1.8
201127519	11.6	6.179	2752.55	2.5	0.01303	11.6	⋯
201128338	13.1	32.655	2775.62	4.0	0.00159	6.7	15.6 ± 2.2
201132684	11.7	10.061	2757.49	3.8	0.00070	8.7	13.8 ± 1.3
201132684	11.7	5.906	2750.82	5.0	0.00015	9.7	13.8 ± 1.3
201164625	11.9	2.711	2750.15	3.1	0.00020	6.7	12.5 ± 1.5
201166680	10.9	24.941	2751.51	5.2	0.00019	6.6	⋯
201166680	10.9	11.540	2760.22	3.7	0.00016	7.8	⋯
201180665	13.1	17.773	2753.50	2.9	0.03662	11.2	⋯
201211526	11.7	21.070	2755.48	3.9	0.00030	8.3	⋯
201225286	11.7	12.420	2753.52	3.3	0.00065	11.6	20.8 ± 1.6
201274010	13.9	13.008	2756.51	2.2	0.00065	7.7	⋯
201352100	12.8	13.383	2761.79	2.2	0.00120	12.5	36 ± 11
201357643	12.0	11.893	2754.55	4.2	0.00107	12.3	⋯
201386739	14.4	5.767	2750.70	3.4	0.00134	11.1	35 ± 6
201390048	12.0	9.455	2750.92	3.0	0.02669	7.7	⋯
201390927	14.2	2.638	2750.34	1.7	0.00110	12.9	⋯
201392505	13.4	27.463	2759.08	5.5	0.00150	9.3	⋯
201437844	9.2	21.057	2757.07	4.4	0.00100	10.0	⋯
201437844	9.2	9.560	2753.52	3.5	0.00030	9.8	⋯
201595106	11.7	0.877	2750.05	1.0	0.00025	9.4	⋯
201598502	14.3	7.515	2755.43	2.3	0.00129	7.5	⋯
201615463	12.0	8.527	2753.77	3.7	0.00016	7.2	⋯
228707509	14.8	15.351	2752.51	3.6	0.02386	13.6	⋯
228720681	13.8	15.782	2753.42	3.4	0.01028	14.3	9.8 ± 1.1
228721452	11.3	4.563	2749.98	2.8	0.00020	12.6	⋯
228721452	11.3	0.506	2750.56	0.9	0.00010	9.6	⋯
228724899	13.3	5.203	2753.45	1.4	0.00113	12.3	⋯
228725791	14.3	6.492	2755.15	1.7	0.00110	9.8	32 ± 3
228725791	14.3	2.251	2749.97	1.2	0.00100	7.3	32 ± 3
228725972	12.5	4.477	2752.69	2.4	0.03270	11.5	⋯
228725972	12.5	10.096	2755.41	3.6	0.05928	13.0	⋯
228729473	11.5	16.773	2752.76	12.4	0.00199	11.6	${36}_{-3}^{+5}$
228732031	11.9	0.369	2749.93	1.0	0.00040	15.1	9.4 ± 1.9
228734900	11.5	15.872	2754.37	4.6	0.00034	8.0	⋯
228735255	12.5	6.569	2755.29	3.3	0.01280	12.6	31.1 ± 2.0
228736155	12.0	3.271	2751.02	2.4	0.00027	9.3	⋯
228739306	13.3	7.172	2755.11	2.8	0.00070	8.1	⋯
228748383	12.5	12.409	2750.04	5.9	0.00024	8.0	⋯
228748826	13.9	4.014	2751.13	2.4	0.00102	13.2	${39}_{-8}^{+6}$
228753871	13.2	18.693	2757.74	2.2	0.00082	7.7	16.4 ± 2.3
228758778	14.8	9.301	2756.07	2.7	0.00214	7.8	⋯
228758948	12.9	12.203	2753.83	4.0	0.00128	12.4	11.3 ± 1.7
228763938	12.6	13.814	2763.19	3.6	0.00036	8.8	⋯
228784812	12.6	4.189	2751.02	2.2	0.00014	8.9	⋯
228798746	12.7	2.697	2750.20	1.5	0.02587	14.1	⋯
228801451	11.0	8.325	2753.35	2.5	0.05325	12.9	19.5 ± 2.7
228801451	11.0	0.584	2750.46	1.5	0.01625	10.0	19.5 ± 2.7
228804845	12.6	2.860	2749.60	2.6	0.00020	7.3	⋯
228809391	12.6	19.580	2763.80	2.6	0.00100	8.3	⋯
228809550	14.7	4.002	2751.00	2.1	0.01259	12.5	⋯
228834632	14.9	11.730	2758.63	2.1	0.00111	8.6	23.6 ± 2.1
228836835	14.9	0.728	2750.26	0.8	0.00068	15.4	⋯
228846243	14.5	25.554	2756.93	5.4	0.00220	10.5	⋯
228849382	13.8	12.120	2757.61	2.4	0.00120	7.6	⋯
228849382	13.8	4.097	2749.96	1.6	0.00052	8.8	⋯
228888935	14.1	5.691	2751.67	3.3	0.00533	10.3	7.2 ± 1.1
228894622	13.3	1.964	2750.31	1.1	0.00183	16.3	20.8 ± 2.4
228934525	13.4	3.676	2752.05	1.7	0.00110	14.2	28.3 ± 3.1
228934525	13.4	7.955	2751.34	2.1	0.00110	11.4	28.3 ± 3.1
228964773	14.9	37.209	2776.76	3.1	0.00280	6.9	⋯
228968232	14.7	5.520	2753.52	3.6	0.00097	8.6	⋯
228974324	12.9	1.606	2750.29	1.3	0.00034	13.1	22.0 ± 2.3
228974907	9.3	20.782	2759.64	5.0	0.00010	7.2	⋯
229004835	10.2	16.138	2764.63	2.1	0.00036	10.6	22.2 ± 2.5
229017395	13.2	19.099	2753.28	6.0	0.00049	8.1	⋯
229103251	13.7	11.667	2756.72	3.1	0.00114	9.9	⋯
229131722	12.5	15.480	2752.71	4.2	0.00037	8.3	⋯
229133720	11.5	4.037	2750.96	1.5	0.00091	12.4	11.8 ± 1.3

Note. Kp denotes magnitude in the Kepler bandpass.

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We used the orbital period, mid-transit time, transit depth, and transit duration identified by BLS as the starting points for more detailed transit modeling. The transit light curve was generated by the Python package batman (Kreidberg 2015). To reduce the data volume, we only use the light curve in a $3\times {T}_{14}$ window centered on the mid-transit times. We first tested if any of the systems showed strong transit timing variations (TTVs). We used the Python interface to the Levenberg–Marquardt nonlinear least squares algorithm lmfit (Newville et al. 2014) to find the best-fit model of the phase-folded transit, and then fit this template to each transit separately to identify individual transit times of each candidate. Since none of the system presented in this work showed significant TTVs within the K2 C10 observations, we assumed linear ephemerides in subsequent analyses.

The transit parameters in our linear ephemeris model include the orbital period P_orb, the mid-transit time T₀, the planet-to-star radius ratio ${R}_{p}$/${R}_{\star }$, the scaled orbital distance a/${R}_{\star }$, the impact parameter $b\equiv a\cos i/{R}_{\star }$, and the transformed quadratic limb-darkening coefficients q₁ and q₂. Instead of fixing the parameters of the quadratic limb-darkening law to theoretical values based on stellar models, in this work we opt to allow these parameters to vary, as this allows for error propagation from stellar uncertainties. We utilize the available stellar parameters and their uncertainties to impose Gaussian priors on the limb-darkening coefficients (i.e., in the non-transformed parameter space, u₁ and u₂). To determine the location and width of these priors, we used a Monte Carlo method to sample the stellar parameters of each candidate host star (${T}_{\mathrm{eff}}$, $\mathrm{log}g$, and $[{\rm{Fe}}/{\rm{H}}]$), and then used these to derive distributions of u₁ and u₂ from an interpolated grid based on the limb-darkening coefficients for the Kepler bandpass tabulated by Claret et al. (2012). We used the median and standard deviation of these distributions to define the Gaussian limb-darkening priors, and used uniform priors for all other parameters. Depending on the uncertainty in the stellar parameters, the limb-darkening priors determined in this way have typical widths of ∼10%, which is comparable to the uncertainty in the models used to predict them (e.g., Csizmadia et al. 2013; Müller et al. 2013). In addition, when the stars are active we do not expect agreement between theoretical and observed limb darkening because the tabulated theoretical values do not take into account the effects of stellar spots and faculae (Csizmadia et al. 2013). To account for the 30 minutes integration time of long-cadence K2 photometry, we used the built-in feature of batman to super-sample the model light curve by a factor of 16 before averaging every 3 minutes window (Kipping 2010).

We adopted a Gaussian likelihood function and found the maximum likelihood solution using scipy.optimize (Jones et al. 2001). We then sampled the joint posterior distribution using emcee (Foreman-Mackey et al. 2013), a Python implementation of the affine-invariant Markov Chain Monte Carlo ensemble sampler (Goodman & Weare 2010). We assumed the errors to be Gaussian, independent, and identically distributed, and thus described by a single parameter. In the maximum likelihood fits, we fixed the value of this parameter to the standard deviation of the out of transit flux, and during MCMC we fit for this value as a free parameter. We launched 100 walkers in the vicinity of the maximum likelihood solution and ran the sampler for 5000 steps, discarding the first 1000 as "burn-in." To ensure that the resultant marginalized posterior distributions consisted of 1000's of independent samples (enough for negligible sampling error) we computed the autocorrelation time of each parameter, and visual inspection revealed the posteriors to be smooth and unimodal. We summarize the transit parameter posterior distributions in Table 5 using the 16th, 50th, and 84th percentiles, and we use the posterior samples to compute other quantities of interest throughout this work (i.e., ${R}_{p}$, ${T}_{\mathrm{eq}}$). The phase-folded light curves of the candidates are shown in Figure 1, with best-fitting transit model and 1σ (68%) credible region overplotted.

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Most of the high-resolution spectra presented in this paper were obtained with the Tull Coudé cross-dispersed echelle spectrograph (Tull et al. 1995) at the Harlan J. Smith 2.7 m telescope at McDonald Observatory. Observations were conducted with the 1.2 × 82 slit, yielding a resolving power of R ∼ 60000. The spectra cover 375–1020 nm, with increasingly larger inter-order gaps long-ward of 570 nm. For each target star, we obtained three successive short exposures in order to allow removal of energetic particle hits on the CCD detector. We used an exposure meter to obtain an accurate flux-weighted barycentric correction and to give an exposure length that resulted in a signal/noise ratio of about 30 per pixel. Bracketing exposures of a Th–Ar hollow cathode lamp were obtained in order to generate a wavelength calibration and to remove spectrograph drifts. This enabled calculation of absolute radial velocities from the spectra. The raw data were processed using IRAF routines to remove the bias level, inter-order scattered light, and pixel-to-pixel ("flat field") CCD sensitivity variations. We traced the apertures for each spectral order and used an optimal extraction algorithm to obtain the detected stellar flux as a function of wavelength.

We computed stellar parameters from our reconnaissance Tull spectra using Kea (Endl & Cochran 2016). In brief, we used standard IRAF routines to perform flat fielding, bias subtraction, and order extraction, and we used a blaze function determined from high signal-to-noise ratio (S/N) flat field exposures to correct for curvature induced by the blaze. Kea uses a large grid of synthetic model stellar spectra to compute stellar effective temperatures, surface gravities, and metallicities. See Table 6 for the stellar parameters used in this work. From a comparison with higher S/N spectra obtained with Keck/HIRES, we found typical uncertainties of 100 K in ${T}_{\mathrm{eff}}$, 0.12 dex in $[{\rm{Fe}}/{\rm{H}}]$, and 0.18 dex in $\mathrm{log}g$. For a detailed description of Kea, see Endl & Cochran (2016).

We also used the FIber-fed Échelle Spectrograph (FIES; Frandsen & Lindberg 1999; Telting et al. 2014) on the 2.56 m Nordic Optical Telescope (NOT) of Roque de los Muchachos Observatory (La Palma, Spain) to collect high-resolution ($R\,\approx \,67\,000$) spectra of four C10 candidate host stars: 228729473, 228735255 (K2-140; Giles et al. 2018, Korth et al., submitted to MNRAS), 201127519, and 228732031 (K2-131; Dai et al. 2017). The observations were carried out between 2017 February 15 and May 23 UTC, within observing programs 54-027, 55-019, and 55-202. We followed the same strategy as in Gandolfi et al. (2013) and traced the RV drift of the instrument by bracketing the science exposures with 90 s ThAr spectra. We reduced the data using standard IRAF routines and extracted the RVs via multi-order cross-correlations using different RV standard stars observed with the same instrument.

We observed the stars 228801451, 228732031 (K2-131; Dai et al. 2017), 201595106, and 201437844 (HD 106315; Crossfield et al. 2017; Rodriguez et al. 2017) with the HARPS-N spectrograph ($R\,\approx$ 115,000; Cosentino et al. 2012) mounted at the 3.58 m Telescopio Nazionale Galileo (TNG) of Roque de los Muchachos Observatory (La Palma, Spain). The observations were performed in 2017 January as part of observing programs A34TAC_10 and A34TAC_44. We reduced the data using the dedicated off-line pipeline and extracted the RVs by cross-correlating the échelle spectra with a G2 numerical mask. The HARPS-N data of 228732031 have been published by our team in Dai et al. (2017). We refer the reader to that paper for a detailed description and analysis of the data. We list the results of our analysis of these spectra in Table 10.

We obtained spectra for 27 candidate host stars in this work, from which we derived ${T}_{\mathrm{eff}}$, $\mathrm{log}g$, $[{\rm{Fe}}/{\rm{H}}]$, and $v\sin i$, as described in Section 4.1. We augment this set of spectroscopic stellar parameters with values from the literature for an additional 14 candidate host stars (Rodriguez et al. 2017; Hirano et al. 2018a; Mayo et al. 2018). To maximize both the quality and uniformity of the final set of stellar parameters we use in this work, we adopted the following strategy. First, we gathered 2MASS JHK photometry and Gaia DR2 parallaxes for all stars; 2MASS photometry is available in the EPIC, and we cross-matched to Gaia DR2 using both position and optical magnitude agreement (Kp and Gaia G band). We then used the isochrones (Morton 2015a) interface to the Dartmouth stellar model grid (Dotter et al. 2008) to estimate stellar parameters and their uncertainties using the MultiNest sampling algorithm (Feroz et al. 2013). For those stars with parameters from spectroscopic analyses, we imposed Gaussian priors on ${T}_{\mathrm{eff}}$, $\mathrm{log}g$, and $[{\rm{Fe}}/{\rm{H}}]$, with mean and standard deviation set by the spectroscopically derived values and their uncertainties. We also ran the same analysis without including parallax, as a check on the quality of the parameters derived in this manner without any distance information; unsurprisingly, we found that including parallax yielded the biggest improvement for stars lacking spectroscopy. This is perhaps most important for the M dwarfs in our sample, which suffer from systematically underestimated radii in the EPIC (see, e.g., Dressing et al. 2017).

As an additional quality check, we also performed spectral analyses for the targets 201127519, 201437844, 201595106, and 228801451, using spectra from FIES and HARPS-N and SpecMatch-emp (Yee et al. 2017). SpecMatch-emp fits the input spectra to hundreds of library template spectra collected by the California Planet Search, and the stellar parameters (${T}_{\mathrm{eff}}$, ${R}_{\star }$, and $[{\rm{Fe}}/{\rm{H}}]$) are estimated based on the interpolation of the parameters for best-matched library stars. Among them, 201127519, 201595106, and 228801451 were also observed with the Tull spectrograph, and the resulting parameters by SpecMatch-emp are in agreement within ∼1.5σ with those estimated from the Tull spectra by the Kea code. For HD 106315, we obtained ${T}_{\mathrm{eff}}$ = 6326 ± 110 K, ${R}_{\star }$ = 1.86 ± 0.30 R_⊙, and $[{\rm{Fe}}/{\rm{H}}]$ = −0.20 ± 0.08. While ${T}_{\mathrm{eff}}$ and $[{\rm{Fe}}/{\rm{H}}]$ agrees within 1σ with the literature values (Crossfield et al. 2017; Rodriguez et al. 2017), ${R}_{\star }$ exhibits a moderate disagreement with that in the literature (${R}_{\star }$ = ${1.281}_{-0.058}^{+0.051}$ R_⊙ Rodriguez et al. 2017). This is probably due to the small number of library stars in SpecMatch-emp in the region with ${T}_{\mathrm{eff}}$ > 6300 K, but this disagreement does not have any impact on our results.

We use the open source vespa software package (Morton 2012, 2015b) to compute the false positive probabilities (FPPs) of each planet candidate. vespa uses the TRILEGAL Galaxy model (Girardi et al. 2005) to compute the posterior probabilities of both planetary and non-planetary scenarios given the observational constraints, and considers false positive scenarios involving simple eclipsing binaries, blended background eclipsing binaries, and hierarchical triple systems. vespa models the physical properties of the host star, taking into account any available broadband photometry and spectroscopic stellar parameters, and compares a large number of simulated scenarios to the observed phase-folded light curve. Both the size of the photometric aperture and contrast curve constraints are accounted for in the calculations, as well as any other observational constraints such as the maximum depth of secondary eclipses allowed by the data. We adopt a fiducial validation criterion of FPP < 0.01, which is reasonably conservative and also consistent with the literature (e.g., Montet et al. 2015; Crossfield et al. 2016; Morton et al. 2016). vespa utilizes the contrast curves derived from the observations listed in Table 9 and described in Section 3. To minimize the possibility of errors in the vespa calculations induced by zero-point offsets or underestimated uncertainties in broadband photometry, we opt to use only the well-calibrated 2MASS JHK magnitudes and their uncertainties, taken from the EPIC, in addition to the Kepler band magnitude required by vespa. The stellar parameters used as input to vespa are identical to those used in our uniform isochrones analysis (see Section 4.4). In addition to stellar parameters, vespa utilizes basic system properties (i.e., R.A., decl., P_orb, ${R}_{p}$/${R}_{\star }$), as well as contrast curves (see Section 3) and constraints on secondary eclipse depth and maximum exclusion radii (see Table 8). We tabulate candidate parameters along with their FPPs and final dispositions in Table 5, and the full vespa likelihoods are listed in Table 7. We denote final dispositions as follows: "VP" = validated planet; "PC" = planet candidate; "FP" = false positive.

All of the candidates we detect in multi-planet systems meet the fiducial validation criterion of FPP < 1%. However, FPPs computed with vespa treat only the individual planet candidates in isolation and thus do not take into account any multiplicity in each system. Stars with multiple transiting planet candidates have been shown to exhibit a lower false positive rate by an order of magnitude (Lissauer et al. 2011, 2012, 2014). For this reason, we apply a "multiplicity boost" factor to the planet probability appropriate for each candidate in a multi-planet system. Lissauer et al. (2012) estimated a multiplicity boost factor of 25 for systems containing two planet candidates in the Kepler field, and we apply the same factor in this work. To check that this factor is appropriate for K2 C10, we follow Sinukoff et al. (2016) and utilize Equations (2) and (4) of Lissauer et al. (2012) to estimate the sample purity P from the integrated FPP of our sample and the number of planet candidates we detect (72). This estimate of P is quite high, perhaps due to a lack of contamination from background stars due to the high galactic latitude of the field, or due to our team's vetting procedures. The fraction of detected planet candidates in multi-systems (18/72) in conjunction with the high sample purity yields a multiplicity boost which is significantly higher than the factor of 25 estimated by Lissauer et al. (2012) for the Kepler field. Although the true value is likely to be higher, we conservatively apply only a factor of 25, consistent with Lissauer et al. (2012), and the FPPs in Table 5 reflect this accordingly.

To ensure that the FPPs computed by vespa are reliable, we take into account the presence of any nearby stars detected in speckle or archival imaging. Table 2 lists the nearby stars we detected via speckle imagine, along with their separations and delta-magnitudes relative to the primary stars. Figure 3 shows the reconstructed speckle images for these stars, and Figure 2 shows these detections relative to the ensemble of contrast curves from all of our speckle images. Table 3 lists those stars found in the EPIC to be near and bright enough to be the source of the observed transit signals.

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5.2.1. Companions Detected in High-resolution Imaging

On the nights of 2017 March 15, 17, and 18 we acquired speckle imaging of the stars 201352100, 201390927, 201392505, and 228964773 (see Table 9). We detected companions in the reconstructed images (see Figure 3), so we assessed the possibility that the transit signal might not originate from the primary stars. We used the following relation between the observed transit depth $\delta ^{\prime}$ and the true transit depth δ in the presence of dilution from a companion ${\rm{\Delta }}m$ magnitudes fainter than the primary star:

$$\begin{eqnarray}&&\delta ^{\prime} =\displaystyle \frac{\delta }{1+{10}^{0.4{\rm{\Delta }}m}}.\end{eqnarray} \tag{ 1 }$$

Assuming a maximum eclipse depth of 100% (i.e., a brown dwarf—M dwarf binary) we can potentially rule out the secondary star as the source of the observed signal. For shallower transits the maximum allowed dilution from the primary is larger, and therefore even a relatively faint secondary source cannot be ruled out as the host. For each of these four candidates, the secondary source is bright enough (given the observed transit depth) that we cannot rule out the possibility they are the source of the signal (see Table 2). For this reason, we do not validate any of these candidates as planets, as we do not know the true source of the signal (and therefore the true planet size), even though they all have low FPPs.

5.2.2. Companions in the EPIC

5.2.3. Archival Imaging

As a check on the accuracy of the sources comprising the EPIC, we also queried 1' × 1' Pan-STARRS-1²⁵ grizy images centered at the position of each candidate host star. We found good agreement with the catalog query: nearby stars found by the catalog query were clearly visible in the images, and no nearby bright sources were seen in the images that were not previously found by the catalog query. We show these images in Figure 4, with overplotted circular regions illustrating the size and location of the apertures used to extract photometry from the K2 pixel data.

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In light of several recent cases of contamination from false positives in statistically validated planet samples (Cabrera et al. 2017; Shporer et al. 2017), we also scrutinized our candidates at the pixel level. To do so, we extracted light curves from different sized apertures and looked for signs of a dependence of transit depth on aperture radius. In some cases, these light curves are too noisy to draw conclusions from, as they are extracted from "non-optimal" apertures. However, this analysis is especially important when there are widely separated neighboring stars (i.e., several Kepler pixels away) that still contribute flux to the K2 apertures, in which case it may be possible to determine the origin of the transit-like signal by this method. Based on these analyses we found that the transit signal associated with the candidate 201164625.01 most likely originates from the neighboring star, 201164669 (see Table 3 and Figure 4). We also detected suspicious transit depth behavior in the light curves of 201392505.01 and 228964773.01, both of which have nearby companions detected in speckle imaging. Intriguingly, these companions are well within a Kepler pixel of the target star, so even the smallest aperture possible (one Kepler pixel) should contain light from both the primary and secondary stars. This result may indicate the presence of another (undetected) star further away, and suggests that such multi-aperture analyses should be useful for ranking the quality of candidates when high-resolution imaging is unavailable.

As a final step in the validation process, we compute the transit S/N for each candidate in order to enforce a minimum transit quality standard for all planets in the validated sample. We compute the transit S/N using the simple approximation that the signal scales with the transit depth and the square root of the number of transits (e.g., Bouma et al. 2017). We estimate the noise by computing the standard deviation of the out-of-transit photometry used in our light curve fits and scaling it from the K2 observing cadence to the transit duration of each candidate. We find median S/N values of 17.1 and 17.6 for the validated and candidate samples, respectively. The slightly lower S/N of the validated sample is likely attributable to the fact that candidates with higher FPPs are typically larger and have correspondingly deeper transits, whereas the vast majority of our validated planets are sub-Neptunes (see Figure 5). Our validated sample consists of planets with S/N > 10, with the exception of K2-254 b and K2-247 c, which have S/N values of 6.7 and 8.9, respectively. However, these are both in multi-planet systems, which increases our confidence in the veracity of the transit signals. We argue that candidates with relatively low S/N found in systems with multiple validated candidates need not be regarded with as much suspicion as similarly low-S/N candidates in single-candidate systems; this is related to, but more qualitative than, the "multi-boost" argument of Lissauer et al. (2012). Indeed, many interesting planets with low S/N likely remain to be found in both the Kepler and K2 data (e.g., Shallue & Vanderburg 2018).

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To check the quality of our light curves and provide an additional layer of confidence in our candidates, we performed a parallel analysis using light curves from an independent K2 pipeline. We first downloaded the light curves of Vanderburg & Johnson (2014) from MAST for all the targets listed in Table 1, then detrended the light curves by fitting a second order polynomial to the out-of-transit data using exotrending (Barragán & Gandolfi 2017). To explore the transit model parameter space with MCMC, we used pyaneti (Barragán et al. 2017) to fit the detrended light curves with uniform priors for all parameters; more description of the pyaneti MCMC evolution and parameter estimation can be found in Barragán et al. (2018) and Gandolfi et al. (2017). For the majority of candidates, the main transit parameters of interest (P_orb, ${R}_{p}$/${R}_{\star }$, b, and a/${R}_{\star }$) are consistent within 1σ between our two independent analyses, although there are some cases in which marginally significant differences were found. These differences are likely to be the result of different handling of the K2 systematics and/or the stellar variability in the light curves. The overall good agreement between these two independently derived sets of transit parameters provides an additional layer of confidence in the quality of the candidates. The results of this comparison are listed in Table 12.

We validate 44 planets out of our sample of 72 candidates, and tabulate the FPPs along with parameter estimates of interest in Table 5. Of the 44 validated planets we report here, 20 of them have been previously statistically validated or confirmed: 201598502.01, 228934525.01, and 228934525.02 (K2-153 b, K2-154 bc; Hirano et al. 2018a); 228735255.01 (K2-140 b; Giles et al. 2018, Korth et al., submitted to MNRAS); 201437844.01 and 201437844.02 (HD 106315bc; Crossfield et al. 2017; Rodriguez et al. 2017); 228732031.01 (K2-131 b; Dai et al. 2017); and 13 others were recently validated by Mayo et al. (2018). In the left panel of Figure 5 we plot the planetary radii, orbital periods, and equilibrium temperatures of the validated planets in the sample.

We investigated the impact of these new planets to the population of currently known planets by querying the NASA Exoplanet Archive²⁶ (Akeson et al. 2013). We computed the fractional enhancement to the known population due to the 44 planets as a function of planet size and host star brightness (see Figure 6). As of 2018 June 12, the populations of super-Earths (${R}_{p}$ ≈ 1–2${R}_{\oplus }$), sub-Neptunes (${R}_{p}$ ≈ 2–4${R}_{\oplus }$), and sub-Saturns (${R}_{p}$ ≈ 4–8${R}_{\oplus }$) orbiting bright stars (J = 8–10 mag) are enhanced by ∼4%, ∼17%, and ∼11%, respectively. Because of the brightness of the host stars, many of these planets are ideal for detailed characterization studies via precision Doppler and transmission spectroscopy, which we discuss in greater detail in Section 6.4.

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Out of the 72 planet candidates we present here, 27 are not validated. Most cannot be validated due to the FPP being above our fiducial validation criterion of 1% or the presence of a contaminating star within the photometric aperture. See Table 7 for the likelihoods of various false positive scenarios and the planet scenario, as computed by vespa. There are several candidates which we do not validate for other reasons, which we discuss below. In the right panel of Figure 5, we plot the planetary radii, orbital periods, and equilibrium temperatures of the non-validated candidates.

The candidate 228729473.01 exhibits a long transit duration, and subsequent spectroscopic analyses revealed large RV variations which are consistent with the candidate being a false positive involving an M dwarf eclipsing a sub-giant, see S. Csizmadia et al. (2018, in preparation) for more details. The light curve of 229133720.01 exhibits low levels of variability in phase with the transit signal, which could be due to ellipsoidal variations; thus we do not validate the candidate in spite of its low FPP. Although 201390048.01 was recently validated (K2-162 b; Mayo et al. 2018), we found marginal evidence of odd–even variations in the light curve of this candidate, which could be an indication that the signal is actually caused by an eclipsing binary at twice the estimated orbital period. Although vespa accounts for this scenario in its FPP calculation, we do not validate the candidate even though its FPP is below 1%. The candidate 201180665.01 has a relatively high FPP (∼64%), and also a suspiciously large radius estimate (∼26 ${R}_{\oplus }$). Although spectroscopic characterization could yield a different radius estimate for the host star (and thus also for the candidate), we conclude that this is most likely an eclipsing M dwarf companion. The candidates 228974907.01, and 228846243.01 do not have particularly low FPPs, but they may be interesting targets for further observations due to their relatively long orbital periods. The candidate 201128338.01 was statistically validated previously in the literature (K2-152 b; Hirano et al. 2018a); we find a similarly low FPP, but we do not validate it simply because it has fewer than three transits in the K2 photometry (and thus odd/even variations in transit depth cannot be robustly ruled out). Further observations will shed light on the true nature of these candidates, either by measuring RV variations with precision spectrographs or via simultaneous multi-band transit observations with instruments such as MuSCAT (Narita et al. 2015) and MuSCAT2 (a griz clone of MuSCAT now in operation at Teide Observatory).

The integrated FPP is ∼2.1 for the full set of 72 candidates, which implies the existence of two false positives in the sample. We have already confirmed that 228729473.01 is a false positive via RV observations (see S. Csizmadia et al. 2018, in preparation), and we suspect 229133720.01, 201390048.01, and 201180665.01 of being false positives, as described above. Therefore, we expect no false positives among the remainder of the sample, and most of the 27 unvalidated candidates could be statistically validated or confirmed by future observations.

6.3.1. Ultra-short Period Planets (USPs)

6.3.2. Multi-planet Systems

We predicted the masses of the candidates using the probabilistic mass–radius relation of Wolfgang et al. (2016) ²⁷ (see Table 5). The predicted masses enabled us to compute other quantities of interest, which we then used to identify potentially interesting targets for follow-up characterization via Doppler and transmission spectroscopy.

6.4.1. Doppler Targets

We computed the expected Doppler semi-amplitude due to the reflex motion of the host star induced by each planet (see Table 5). We used these expected semi-amplitudes in conjunction with the brightness of the host stars to identify planets in the sample which are good targets for radial velocity (RV) follow-up study using current and future facilities. Such RV observations will reveal the planets' densities and constrain their bulk compositions. This is of particular interest for relatively small planets with radii in the range 1.5–2.5 ${R}_{\oplus }$ because such measurements could enable tests of planet formation theories and post-processes, such as the photoevaporation (e.g., Owen & Wu 2013; Lopez & Fortney 2014), which has been proposed to explain the observed gap in the radius distribution (Fulton et al. 2017; Van Eylen et al. 2018a). However, because of the difficulty of detecting the small Doppler signals of such planets, it is especially important to identify such planets which are orbiting relatively bright stars, for which the RV precision required to measure their masses is more readily obtainable. Table 4 lists validated planets with predicted Doppler semi-amplitudes greater than 1 m s⁻¹ orbiting stars brighter than Kp = 12 mag. For convenience, we also list planetary orbital periods and stellar rotational periods (when available); potentially confounding quasi-periodic RV signals produced by stellar magnetic activity are less likely to present a challenge for mass measurement when the orbital period is far from the stellar rotational period (or a harmonic). We note that 228732031.01 (K2-131 b) and 228801451.01 (K2-229 b) both already have measured masses via precision RVs (Dai et al. 2017; Santerne et al. 2018).

Table 4.  Validated Planets with Predicted Doppler Semi-amplitudes Greater than 1 m s⁻¹ Orbiting Stars Brighter than Kp = 12 mag

EPIC	Kp	Kpred	${R}_{p}$	Porb	Prot
	(mag)	(m s−1)	(${R}_{\oplus }$)	(days)	(days)
201092629.01	11.858	${2.5}_{-0.7}^{+0.7}$	2.55	26.8199	${22}_{-2}^{+6}$
201132684.01	11.678	${3.0}_{-0.8}^{+0.8}$	2.64	10.0605	13.8 ± 1.3
201132684.02	11.678	${1.3}_{-0.7}^{+0.7}$	1.28	5.9028	13.8 ± 1.3
201166680.02	10.897	${1.8}_{-0.6}^{+0.6}$	2.17	11.5418	⋯
201166680.03	10.897	${1.2}_{-0.4}^{+0.5}$	2.01	24.9460	⋯
201211526.01	11.696	${1.5}_{-0.6}^{+0.6}$	1.75	21.0688	⋯
201225286.01	11.729	${2.3}_{-0.7}^{+0.7}$	2.26	12.4220	20.8 ± 1.6
201357643.01	11.998	${5.7}_{-1.1}^{+1.2}$	4.34	11.8931	⋯
201437844.01	9.234	${2.3}_{-0.7}^{+0.7}$	2.32	9.5580	⋯
201437844.02	9.234	${3.9}_{-0.7}^{+0.8}$	4.31	21.0579	⋯
201615463.01	11.964	${2.1}_{-0.7}^{+0.7}$	2.19	8.5270	⋯
228721452.02	11.325	${1.8}_{-0.8}^{+0.9}$	1.57	4.5633	⋯
228732031.01	11.937	${5.3}_{-2.2}^{+2.3}$	1.70	0.3693	9.4 ± 1.9
228734900.01	11.535	${2.9}_{-0.6}^{+0.7}$	3.49	15.8721	⋯
228801451.01	10.955	${2.2}_{-1.2}^{+1.0}$	1.14	0.5843	19.5 ± 2.7
228801451.02	10.955	${2.3}_{-0.8}^{+0.8}$	2.03	8.3273	19.5 ± 2.7

Note. 228721452.01 is not listed here because it does not meet these criteria, but RV measurements to constrain the mass of 228721452.02 could also reveal the inner planet's mass, as both Keplerian signals would need to be accounted for in the RV analysis.

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Table 5.  Planet and Candidate Parameters

EPIC	Name	Porb	T0	a	b	${R}_{p}$	a	${R}_{p}$	${T}_{\mathrm{eq}}$	MP	Kpred	${\rho }_{\star ,\mathrm{LC}}$	FPP	Disposition
		(days)	(BKJD)	(${R}_{\star }$)		(${R}_{\star }$)	(au)	(${R}_{\oplus }$)	(K)	(${M}_{\oplus }$)	(m s−1)	$({\rho }_{\odot })$
201092629.01	K2-241 b	${26.81990}_{-0.00247}^{+0.00245}$	${2751.2063}_{-0.0034}^{+0.0035}$	${43.3}_{-9.9}^{+3.8}$	${0.41}_{-0.28}^{+0.30}$	${0.0312}_{-0.0012}^{+0.0023}$	${0.1567}_{-0.0008}^{+0.0007}$	${2.55}_{-0.10}^{+0.18}$	${507}_{-5}^{+5}$	${9.1}_{-2.4}^{+2.4}$	${2.4}_{-0.7}^{+0.7}$	${1.5}_{-0.8}^{+0.4}$	$7\times {10}^{-8}$	VP
201102594.01	K2-242 b	${6.51389}_{-0.00083}^{+0.00082}$	${2753.2400}_{-0.0054}^{+0.0054}$	${22.1}_{-5.6}^{+3.8}$	${0.42}_{-0.29}^{+0.32}$	${0.0633}_{-0.0044}^{+0.0051}$	${0.0494}_{-0.0004}^{+0.0004}$	${2.54}_{-0.19}^{+0.21}$	${416}_{-8}^{+8}$	${9.0}_{-2.5}^{+2.7}$	${5.9}_{-1.6}^{+1.7}$	${3.4}_{-2.0}^{+2.1}$	$6\times {10}^{-12}$	VP
201110617.01	K2- 156 b	${0.81314}_{-0.00008}^{+0.00007}$	${2750.1427}_{-0.0038}^{+0.0041}$	${4.1}_{-0.9}^{+0.6}$	${0.41}_{-0.27}^{+0.32}$	${0.0161}_{-0.0010}^{+0.0014}$	${0.0149}_{-0.0001}^{+0.0001}$	${1.15}_{-0.07}^{+0.10}$	${1347}_{-19}^{+18}$	${2.7}_{-1.5}^{+1.5}$	${2.4}_{-1.4}^{+1.3}$	${1.4}_{-0.7}^{+0.7}$	$2\times {10}^{-12}$	VP
201111557.01		${2.30183}_{-0.00030}^{+0.00028}$	${2750.1688}_{-0.0052}^{+0.0052}$	${11.8}_{-3.0}^{+2.1}$	${0.42}_{-0.28}^{+0.33}$	${0.0144}_{-0.0010}^{+0.0014}$	${0.0313}_{-0.0004}^{+0.0003}$	${1.12}_{-0.08}^{+0.11}$	${1054}_{-55}^{+55}$	${2.4}_{-1.4}^{+1.6}$	${1.4}_{-0.8}^{+0.9}$	${4.1}_{-2.4}^{+2.6}$	$3\times {10}^{-4}$	PC
201127519.01		${6.17887}_{-0.00007}^{+0.00007}$	${2752.5473}_{-0.0005}^{+0.0005}$	${18.1}_{-0.6}^{+0.2}$	${0.17}_{-0.11}^{+0.14}$	${0.1058}_{-0.0007}^{+0.0011}$	${0.0613}_{-0.0007}^{+0.0007}$	${8.84}_{-0.13}^{+0.14}$	${772}_{-10}^{+10}$	${44.8}_{-12.1}^{+16.2}$	${17.9}_{-4.8}^{+6.6}$	${2.1}_{-0.2}^{+0.1}$	$4\times {10}^{-2}$	PC
201128338.01	K2-152 b	${32.64790}_{-0.01483}^{+0.01141}$	${2775.6222}_{-0.0073}^{+0.0135}$	${58.8}_{-2.9}^{+2.6}$	${0.25}_{-0.17}^{+0.24}$	${0.0344}_{-0.0037}^{+0.0037}$	${0.1716}_{-0.0012}^{+0.0012}$	${2.29}_{-0.24}^{+0.25}$	${337}_{-3}^{+3}$	${8.0}_{-2.7}^{+2.9}$	${2.2}_{-0.7}^{+0.8}$	${2.6}_{-0.4}^{+0.4}$	$1\times {10}^{-7}$	PC
201132684.01	K2-158 b	${10.06049}_{-0.00148}^{+0.00134}$	${2757.4834}_{-0.0064}^{+0.0080}$	${19.1}_{-4.0}^{+1.6}$	${0.38}_{-0.27}^{+0.31}$	${0.0255}_{-0.0008}^{+0.0016}$	${0.0887}_{-0.0008}^{+0.0008}$	${2.64}_{-0.10}^{+0.16}$	${794}_{-11}^{+11}$	${9.6}_{-2.5}^{+2.4}$	${3.0}_{-0.8}^{+0.8}$	${0.9}_{-0.5}^{+0.3}$	$8\times {10}^{-8}$	VP
201132684.02	K2-158 c	${5.90279}_{-0.00233}^{+0.00191}$	${2750.8828}_{-0.0120}^{+0.0131}$	${11.3}_{-2.9}^{+2.4}$	${0.41}_{-0.28}^{+0.34}$	${0.0123}_{-0.0009}^{+0.0012}$	${0.0622}_{-0.0006}^{+0.0006}$	${1.28}_{-0.10}^{+0.13}$	${948}_{-13}^{+13}$	${3.6}_{-1.9}^{+2.0}$	${1.3}_{-0.7}^{+0.8}$	${0.6}_{-0.3}^{+0.4}$	$3\times {10}^{-8}$	VP
201164625.01		${2.71189}_{-0.00056}^{+0.00068}$	${2750.1362}_{-0.0179}^{+0.0112}$	${5.5}_{-1.5}^{+1.1}$	${0.43}_{-0.30}^{+0.35}$	${0.0121}_{-0.0008}^{+0.0010}$	${0.0461}_{-0.0004}^{+0.0004}$	${4.34}_{-0.35}^{+0.43}$	${2336}_{-60}^{+59}$	${17.9}_{-3.8}^{+4.4}$	${5.5}_{-1.2}^{+1.4}$	${0.3}_{-0.2}^{+0.2}$	$4\times {10}^{-3}$	PC
201166680.02	K2-243 b	${11.54182}_{-0.00221}^{+0.00272}$	${2760.2062}_{-0.0102}^{+0.0079}$	${21.2}_{-4.5}^{+2.0}$	${0.39}_{-0.27}^{+0.31}$	${0.0144}_{-0.0007}^{+0.0008}$	${0.1087}_{-0.0014}^{+0.0014}$	${2.17}_{-0.12}^{+0.14}$	${1035}_{-35}^{+36}$	${7.4}_{-2.3}^{+2.4}$	${1.8}_{-0.6}^{+0.6}$	${1.0}_{-0.5}^{+0.3}$	$9\times {10}^{-5}$	VP
201166680.03	K2-243 c	${24.94598}_{-0.00561}^{+0.00491}$	${2751.5050}_{-0.0072}^{+0.0077}$	${35.6}_{-9.2}^{+4.0}$	${0.40}_{-0.27}^{+0.34}$	${0.0133}_{-0.0009}^{+0.0009}$	${0.1817}_{-0.0024}^{+0.0022}$	${2.01}_{-0.13}^{+0.15}$	${801}_{-28}^{+27}$	${6.7}_{-2.3}^{+2.4}$	${1.2}_{-0.4}^{+0.4}$	${1.0}_{-0.6}^{+0.4}$	$1\times {10}^{-4}$	VP
201180665.01		${17.77297}_{-0.00009}^{+0.00009}$	${2753.4986}_{-0.0002}^{+0.0002}$	${33.3}_{-0.3}^{+0.3}$	${0.68}_{-0.01}^{+0.01}$	${0.1892}_{-0.0009}^{+0.0008}$	${0.1404}_{-0.0030}^{+0.0029}$	${26.44}_{-0.65}^{+0.65}$	${830}_{-33}^{+34}$	${184.3}_{-79.4}^{+148.7}$	${40.8}_{-17.6}^{+33.0}$	${1.6}_{-0.0}^{+0.0}$	$6\times {10}^{-1}$	PC
201211526.01	K2-244 b	${21.06884}_{-0.00325}^{+0.00320}$	${2755.4749}_{-0.0065}^{+0.0062}$	${38.3}_{-10.1}^{+5.5}$	${0.44}_{-0.30}^{+0.32}$	${0.0174}_{-0.0009}^{+0.0013}$	${0.1418}_{-0.0011}^{+0.0010}$	${1.75}_{-0.10}^{+0.13}$	${638}_{-7}^{+7}$	${5.7}_{-2.3}^{+2.4}$	${1.5}_{-0.6}^{+0.6}$	${1.7}_{-1.0}^{+0.8}$	$7\times {10}^{-4}$	VP
201225286.01	K2-159 b	${12.42205}_{-0.00182}^{+0.00180}$	${2753.5082}_{-0.0077}^{+0.0074}$	${27.9}_{-6.9}^{+3.8}$	${0.44}_{-0.30}^{+0.30}$	${0.0250}_{-0.0011}^{+0.0018}$	${0.1013}_{-0.0009}^{+0.0008}$	${2.26}_{-0.11}^{+0.17}$	${684}_{-8}^{+8}$	${7.9}_{-2.5}^{+2.4}$	${2.3}_{-0.7}^{+0.7}$	${1.9}_{-1.1}^{+0.9}$	$2\times {10}^{-4}$	VP
201274010.01		${13.01130}_{-0.00422}^{+0.00520}$	${2756.5150}_{-0.0123}^{+0.0086}$	${26.7}_{-6.3}^{+5.8}$	${0.42}_{-0.29}^{+0.31}$	${0.0255}_{-0.0024}^{+0.0025}$	${0.1062}_{-0.0013}^{+0.0013}$	${2.43}_{-0.24}^{+0.25}$	${713}_{-21}^{+21}$	${8.5}_{-2.7}^{+2.5}$	${2.4}_{-0.8}^{+0.7}$	${1.5}_{-0.8}^{+1.2}$	$9\times {10}^{-2}$	PC
201352100.01		${13.38382}_{-0.00114}^{+0.00116}$	${2761.7895}_{-0.0033}^{+0.0032}$	${33.9}_{-7.0}^{+2.8}$	${0.38}_{-0.27}^{+0.30}$	${0.0326}_{-0.0011}^{+0.0020}$	${0.1038}_{-0.0006}^{+0.0007}$	${2.70}_{-0.10}^{+0.17}$	${608}_{-9}^{+9}$	${9.8}_{-2.5}^{+2.4}$	${3.0}_{-0.8}^{+0.7}$	${2.9}_{-1.5}^{+0.8}$	$2\times {10}^{-3}$	PC
201357643.01	K2-245 b	${11.89307}_{-0.00063}^{+0.00065}$	${2754.5524}_{-0.0018}^{+0.0018}$	${17.5}_{-3.1}^{+1.2}$	${0.38}_{-0.26}^{+0.28}$	${0.0317}_{-0.0006}^{+0.0013}$	${0.0959}_{-0.0006}^{+0.0006}$	${4.34}_{-0.14}^{+0.19}$	${923}_{-14}^{+14}$	${18.0}_{-3.4}^{+3.8}$	${5.7}_{-1.1}^{+1.2}$	${0.5}_{-0.2}^{+0.1}$	$2\times {10}^{-4}$	VP
201386739.01	K2-246 b	${5.76918}_{-0.00082}^{+0.00081}$	${2750.6761}_{-0.0062}^{+0.0064}$	${11.1}_{-2.3}^{+1.1}$	${0.41}_{-0.27}^{+0.29}$	${0.0341}_{-0.0017}^{+0.0021}$	${0.0602}_{-0.0004}^{+0.0004}$	${3.49}_{-0.21}^{+0.25}$	${977}_{-18}^{+19}$	${13.6}_{-2.8}^{+3.0}$	${5.3}_{-1.1}^{+1.2}$	${0.5}_{-0.3}^{+0.2}$	$6\times {10}^{-5}$	VP
201390048.01	K2-162 b	${9.45889}_{-0.00107}^{+0.00104}$	${2750.9076}_{-0.0042}^{+0.0047}$	${23.6}_{-5.0}^{+2.4}$	${0.41}_{-0.29}^{+0.30}$	${0.0190}_{-0.0009}^{+0.0014}$	${0.0795}_{-0.0006}^{+0.0006}$	${1.44}_{-0.07}^{+0.11}$	${631}_{-8}^{+8}$	${4.5}_{-2.2}^{+2.3}$	${1.6}_{-0.8}^{+0.9}$	${2.0}_{-1.0}^{+0.7}$	$2\times {10}^{-3}$	PC
201390927.01		${2.63800}_{-0.00029}^{+0.00030}$	${2750.3409}_{-0.0046}^{+0.0042}$	${10.9}_{-2.9}^{+1.6}$	${0.42}_{-0.28}^{+0.33}$	${0.0265}_{-0.0019}^{+0.0025}$	${0.0370}_{-0.0012}^{+0.0011}$	${2.91}_{-0.33}^{+0.40}$	${1313}_{-88}^{+90}$	${10.8}_{-2.9}^{+3.1}$	${5.1}_{-1.4}^{+1.6}$	${2.5}_{-1.5}^{+1.3}$	$3\times {10}^{-5}$	PC
201392505.01		${27.47083}_{-0.01286}^{+0.01089}$	${2759.0795}_{-0.0163}^{+0.0186}$	${30.9}_{-7.5}^{+3.3}$	${0.40}_{-0.28}^{+0.33}$	${0.0412}_{-0.0021}^{+0.0032}$	${0.1657}_{-0.0017}^{+0.0017}$	${3.36}_{-0.18}^{+0.26}$	${480}_{-7}^{+7}$	${13.0}_{-2.7}^{+3.0}$	${3.2}_{-0.7}^{+0.7}$	${0.5}_{-0.3}^{+0.2}$	$7\times {10}^{-8}$	PC
201437844.01	HD 106315 b	${9.55804}_{-0.00170}^{+0.00165}$	${2753.5267}_{-0.0068}^{+0.0067}$	${17.7}_{-4.4}^{+1.6}$	${0.40}_{-0.28}^{+0.33}$	${0.0164}_{-0.0005}^{+0.0009}$	${0.0905}_{-0.0010}^{+0.0010}$	${2.32}_{-0.08}^{+0.13}$	${1046}_{-12}^{+12}$	${8.1}_{-2.4}^{+2.3}$	${2.3}_{-0.7}^{+0.7}$	${0.8}_{-0.5}^{+0.2}$	$4\times {10}^{-4}$	VP
201437844.02	HD 106315 c	${21.05788}_{-0.00133}^{+0.00132}$	${2757.0732}_{-0.0020}^{+0.0021}$	${34.7}_{-3.5}^{+1.2}$	${0.27}_{-0.19}^{+0.24}$	${0.0305}_{-0.0004}^{+0.0006}$	${0.1533}_{-0.0017}^{+0.0016}$	${4.31}_{-0.08}^{+0.10}$	${804}_{-9}^{+9}$	${17.8}_{-3.4}^{+3.7}$	${3.9}_{-0.7}^{+0.8}$	${1.3}_{-0.3}^{+0.1}$	$4\times {10}^{-5}$	VP
201595106.01		${0.87703}_{-0.00013}^{+0.00011}$	${2750.0513}_{-0.0048}^{+0.0050}$	${5.4}_{-1.3}^{+1.3}$	${0.41}_{-0.28}^{+0.32}$	${0.0114}_{-0.0009}^{+0.0011}$	${0.0181}_{-0.0001}^{+0.0001}$	${1.20}_{-0.10}^{+0.11}$	${1874}_{-16}^{+16}$	${2.9}_{-1.6}^{+1.8}$	${1.9}_{-1.1}^{+1.2}$	${2.7}_{-1.5}^{+2.4}$	$2\times {10}^{-3}$	PC
201598502.01	K2-153 b	${7.51574}_{-0.00240}^{+0.00205}$	${2755.4270}_{-0.0111}^{+0.0134}$	${23.6}_{-6.7}^{+5.5}$	${0.42}_{-0.29}^{+0.35}$	${0.0348}_{-0.0032}^{+0.0037}$	${0.0614}_{-0.0004}^{+0.0004}$	${2.00}_{-0.18}^{+0.21}$	${497}_{-6}^{+6}$	${6.7}_{-2.5}^{+2.6}$	${3.3}_{-1.2}^{+1.3}$	${3.1}_{-2.0}^{+2.7}$	$5\times {10}^{-5}$	VP
201615463.01	K2-166 b	${8.52695}_{-0.00370}^{+0.00362}$	${2753.7635}_{-0.0167}^{+0.0165}$	${11.1}_{-2.6}^{+1.2}$	${0.40}_{-0.28}^{+0.32}$	${0.0124}_{-0.0010}^{+0.0011}$	${0.0858}_{-0.0009}^{+0.0010}$	${2.19}_{-0.19}^{+0.20}$	${1140}_{-18}^{+17}$	${7.4}_{-2.4}^{+2.5}$	${2.1}_{-0.7}^{+0.7}$	${0.3}_{-0.1}^{+0.1}$	$3\times {10}^{-4}$	VP
228707509.01		${15.35092}_{-0.00033}^{+0.00032}$	${2752.5093}_{-0.0009}^{+0.0010}$	${25.3}_{-1.1}^{+1.4}$	${0.63}_{-0.06}^{+0.04}$	${0.1505}_{-0.0031}^{+0.0026}$	${0.1210}_{-0.0029}^{+0.0027}$	${16.31}_{-0.72}^{+0.75}$	${734}_{-33}^{+32}$	${98.8}_{-36.1}^{+59.6}$	${25.4}_{-9.3}^{+15.3}$	${0.9}_{-0.1}^{+0.2}$	$7\times {10}^{-4}$	PC
228720681.01		${15.78132}_{-0.00037}^{+0.00038}$	${2753.4189}_{-0.0010}^{+0.0010}$	${26.1}_{-2.3}^{+4.0}$	${0.68}_{-0.15}^{+0.07}$	${0.0982}_{-0.0035}^{+0.0026}$	${0.1182}_{-0.0014}^{+0.0013}$	${10.87}_{-1.53}^{+1.55}$	${741}_{-54}^{+52}$	${56.7}_{-18.5}^{+29.8}$	${15.7}_{-5.1}^{+8.3}$	${1.0}_{-0.2}^{+0.5}$	$1\times {10}^{-2}$	PC
228721452.01	K2- 223 b	${0.50565}_{-0.00005}^{+0.00006}$	${2750.5640}_{-0.0049}^{+0.0042}$	${3.9}_{-0.9}^{+1.1}$	${0.41}_{-0.28}^{+0.32}$	${0.0083}_{-0.0007}^{+0.0009}$	${0.0127}_{-0.0001}^{+0.0001}$	${0.89}_{-0.08}^{+0.10}$	${2271}_{-23}^{+23}$	${0.9}_{-0.6}^{+0.8}$	${0.7}_{-0.4}^{+0.6}$	${3.0}_{-1.7}^{+3.2}$	$1\times {10}^{-4}$	VP
228721452.02	K2-223 c	${4.56327}_{-0.00049}^{+0.00051}$	${2749.9755}_{-0.0045}^{+0.0044}$	${11.0}_{-2.6}^{+1.2}$	${0.42}_{-0.29}^{+0.30}$	${0.0146}_{-0.0006}^{+0.0010}$	${0.0549}_{-0.0003}^{+0.0003}$	${1.57}_{-0.07}^{+0.11}$	${1091}_{-11}^{+11}$	${5.0}_{-2.2}^{+2.4}$	${1.8}_{-0.8}^{+0.9}$	${0.8}_{-0.5}^{+0.3}$	$2\times {10}^{-6}$	VP
228724899.01		${5.20256}_{-0.00044}^{+0.00042}$	${2753.4559}_{-0.0034}^{+0.0036}$	${26.2}_{-6.5}^{+3.5}$	${0.42}_{-0.29}^{+0.32}$	${0.0338}_{-0.0019}^{+0.0028}$	${0.0578}_{-0.0005}^{+0.0005}$	${3.58}_{-0.20}^{+0.31}$	${1000}_{-14}^{+14}$	${14.1}_{-2.9}^{+3.2}$	${5.4}_{-1.1}^{+1.2}$	${8.9}_{-5.1}^{+4.0}$	$1\times {10}^{-1}$	PC
228725791.01	K2-247 b	${2.25021}_{-0.00036}^{+0.00033}$	${2749.9770}_{-0.0061}^{+0.0064}$	${8.7}_{-2.4}^{+1.5}$	${0.43}_{-0.30}^{+0.34}$	${0.0283}_{-0.0020}^{+0.0025}$	${0.0304}_{-0.0004}^{+0.0004}$	${2.12}_{-0.16}^{+0.19}$	${979}_{-51}^{+52}$	${7.3}_{-2.5}^{+2.5}$	${4.3}_{-1.5}^{+1.5}$	${1.7}_{-1.1}^{+1.1}$	$2\times {10}^{-9}$	VP
228725791.02	K2-247 c	${6.49424}_{-0.00251}^{+0.00260}$	${2755.1369}_{-0.0163}^{+0.0176}$	${18.2}_{-4.7}^{+3.9}$	${0.41}_{-0.28}^{+0.33}$	${0.0292}_{-0.0030}^{+0.0032}$	${0.0615}_{-0.0008}^{+0.0008}$	${2.19}_{-0.23}^{+0.25}$	${688}_{-35}^{+36}$	${7.5}_{-2.5}^{+2.6}$	${3.1}_{-1.1}^{+1.1}$	${1.9}_{-1.1}^{+1.5}$	$1\times {10}^{-7}$	VP
228725972.01	K2-224 b	${4.47904}_{-0.00132}^{+0.00116}$	${2752.6719}_{-0.0111}^{+0.0135}$	${13.2}_{-3.5}^{+2.5}$	${0.41}_{-0.28}^{+0.34}$	${0.0170}_{-0.0015}^{+0.0017}$	${0.0516}_{-0.0004}^{+0.0004}$	${1.56}_{-0.14}^{+0.16}$	${1002}_{-11}^{+11}$	${4.9}_{-2.3}^{+2.4}$	${2.0}_{-0.9}^{+1.0}$	${1.5}_{-0.9}^{+1.1}$	$2\times {10}^{-6}$	VP
228725972.02	K2-224 c	${10.09489}_{-0.00114}^{+0.00119}$	${2755.4157}_{-0.0041}^{+0.0041}$	${20.3}_{-4.5}^{+1.8}$	${0.40}_{-0.27}^{+0.31}$	${0.0262}_{-0.0012}^{+0.0017}$	${0.0886}_{-0.0007}^{+0.0007}$	${2.41}_{-0.12}^{+0.16}$	${764}_{-9}^{+9}$	${8.4}_{-2.5}^{+2.4}$	${2.7}_{-0.8}^{+0.7}$	${1.1}_{-0.6}^{+0.3}$	$9\times {10}^{-6}$	VP
228729473.01		${16.77217}_{-0.00192}^{+0.00185}$	${2752.7609}_{-0.0036}^{+0.0039}$	${6.8}_{-1.0}^{+1.5}$	${0.63}_{-0.34}^{+0.13}$	${0.0448}_{-0.0025}^{+0.0022}$	${0.1367}_{-0.0041}^{+0.0038}$	${19.29}_{-1.11}^{+1.18}$	${1173}_{-27}^{+26}$	${120.7}_{-47.8}^{+80.6}$	${26.4}_{-10.5}^{+17.9}$	$\lt 0.05$	$2\times {10}^{-1}$	FP
228732031.01	K2-131 b	${0.36931}_{-0.00001}^{+0.00001}$	${2749.9355}_{-0.0010}^{+0.0011}$	${2.6}_{-0.4}^{+0.2}$	${0.40}_{-0.26}^{+0.27}$	${0.0207}_{-0.0005}^{+0.0010}$	${0.0095}_{-0.00005}^{+0.00005}$	${1.70}_{-0.05}^{+0.09}$	${2062}_{-23}^{+23}$	${5.5}_{-2.3}^{+2.3}$	${5.4}_{-2.2}^{+2.3}$	${1.7}_{-0.6}^{+0.4}$	$2\times {10}^{-9}$	VP
228734900.01	K2-225 b	${15.87209}_{-0.00338}^{+0.00387}$	${2754.3754}_{-0.0081}^{+0.0091}$	${17.8}_{-4.1}^{+1.9}$	${0.40}_{-0.27}^{+0.32}$	${0.0188}_{-0.0010}^{+0.0013}$	${0.1340}_{-0.0010}^{+0.0010}$	${3.49}_{-0.20}^{+0.26}$	${902}_{-13}^{+13}$	${13.6}_{-2.8}^{+3.1}$	${2.9}_{-0.6}^{+0.7}$	${0.3}_{-0.2}^{+0.1}$	$4\times {10}^{-3}$	VP
228735255.01	K2-140 b	${6.56918}_{-0.00004}^{+0.00004}$	${2755.2851}_{-0.0002}^{+0.0002}$	${15.1}_{-0.3}^{+0.1}$	${0.12}_{-0.08}^{+0.10}$	${0.1130}_{-0.0005}^{+0.0006}$	${0.0687}_{-0.0005}^{+0.0005}$	${12.25}_{-0.17}^{+0.17}$	${957}_{-11}^{+11}$	${67.2}_{-21.4}^{+31.2}$	${22.8}_{-7.3}^{+10.7}$	${1.1}_{-0.1}^{+0.0}$	$1\times {10}^{-14}$	VP
228736155.01	K2-226 b	${3.27108}_{-0.00050}^{+0.00049}$	${2751.0247}_{-0.0059}^{+0.0062}$	${9.7}_{-2.7}^{+1.2}$	${0.45}_{-0.31}^{+0.33}$	${0.0156}_{-0.0009}^{+0.0013}$	${0.0413}_{-0.0005}^{+0.0005}$	${1.54}_{-0.09}^{+0.14}$	${1120}_{-16}^{+16}$	${4.9}_{-2.2}^{+2.4}$	${2.3}_{-1.0}^{+1.1}$	${1.1}_{-0.7}^{+0.5}$	$2\times {10}^{-7}$	VP
228739306.01	K2-248 b	${7.17256}_{-0.00142}^{+0.00148}$	${2755.1042}_{-0.0078}^{+0.0072}$	${16.2}_{-3.9}^{+1.8}$	${0.40}_{-0.28}^{+0.33}$	${0.0255}_{-0.0013}^{+0.0019}$	${0.0699}_{-0.0010}^{+0.0010}$	${2.57}_{-0.14}^{+0.20}$	${886}_{-18}^{+19}$	${9.2}_{-2.4}^{+2.5}$	${3.3}_{-0.9}^{+0.9}$	${1.1}_{-0.6}^{+0.4}$	$6\times {10}^{-5}$	VP
228748383.01	K2-249 b	${12.40900}_{-0.00284}^{+0.00337}$	${2750.0457}_{-0.0113}^{+0.0106}$	${14.5}_{-3.6}^{+1.7}$	${0.41}_{-0.28}^{+0.33}$	${0.0162}_{-0.0011}^{+0.0014}$	${0.1151}_{-0.0031}^{+0.0030}$	${2.79}_{-0.22}^{+0.27}$	${1061}_{-66}^{+66}$	${10.1}_{-2.7}^{+2.8}$	${2.3}_{-0.6}^{+0.6}$	${0.3}_{-0.2}^{+0.1}$	$1\times {10}^{-4}$	VP
228748826.01	K2-250 b	${4.01457}_{-0.00057}^{+0.00062}$	${2751.1212}_{-0.0066}^{+0.0061}$	${12.3}_{-3.0}^{+1.5}$	${0.41}_{-0.28}^{+0.32}$	${0.0276}_{-0.0016}^{+0.0022}$	${0.0459}_{-0.0005}^{+0.0005}$	${2.44}_{-0.15}^{+0.19}$	${958}_{-13}^{+14}$	${8.6}_{-2.5}^{+2.5}$	${4.0}_{-1.1}^{+1.2}$	${1.6}_{-0.9}^{+0.6}$	$3\times {10}^{-5}$	VP
228753871.01		${18.69646}_{-0.00441}^{+0.00447}$	${2757.7290}_{-0.0108}^{+0.0108}$	${65.6}_{-17.2}^{+11.6}$	${0.42}_{-0.29}^{+0.34}$	${0.0278}_{-0.0024}^{+0.0028}$	${0.1302}_{-0.0014}^{+0.0014}$	${2.35}_{-0.20}^{+0.25}$	${571}_{-19}^{+19}$	${8.2}_{-2.6}^{+2.6}$	${2.2}_{-0.7}^{+0.7}$	${10.8}_{-6.5}^{+6.9}$	$7\times {10}^{-2}$	PC
228758778.01	K2-251 b	${9.30075}_{-0.00321}^{+0.00332}$	${2756.0782}_{-0.0108}^{+0.0128}$	${20.6}_{-6.1}^{+4.9}$	${0.44}_{-0.30}^{+0.33}$	${0.0437}_{-0.0038}^{+0.0047}$	${0.0694}_{-0.0005}^{+0.0005}$	${2.35}_{-0.21}^{+0.26}$	${437}_{-9}^{+9}$	${8.2}_{-2.5}^{+2.6}$	${3.9}_{-1.2}^{+1.2}$	${1.4}_{-0.9}^{+1.2}$	$4\times {10}^{-7}$	VP
228758948.01		${12.20239}_{-0.00070}^{+0.00072}$	${2753.8291}_{-0.0023}^{+0.0024}$	${22.2}_{-4.6}^{+1.8}$	${0.40}_{-0.26}^{+0.29}$	${0.0370}_{-0.0010}^{+0.0018}$	${0.1066}_{-0.0006}^{+0.0006}$	${4.15}_{-0.14}^{+0.21}$	${812}_{-9}^{+10}$	${17.0}_{-3.3}^{+3.5}$	${4.5}_{-0.9}^{+0.9}$	${1.0}_{-0.5}^{+0.3}$	$4\times {10}^{-4}$	PC
228763938.01	K2-252 b	${13.81513}_{-0.00448}^{+0.00461}$	${2763.1901}_{-0.0111}^{+0.0118}$	${25.7}_{-6.3}^{+3.5}$	${0.41}_{-0.28}^{+0.32}$	${0.0193}_{-0.0013}^{+0.0018}$	${0.1041}_{-0.0007}^{+0.0008}$	${1.74}_{-0.12}^{+0.17}$	${639}_{-7}^{+7}$	${5.6}_{-2.3}^{+2.4}$	${1.8}_{-0.7}^{+0.7}$	${1.2}_{-0.7}^{+0.6}$	$4\times {10}^{-5}$	VP
228784812.01		${4.18787}_{-0.00137}^{+0.00138}$	${2751.0327}_{-0.0121}^{+0.0115}$	${12.5}_{-0.6}^{+0.6}$	${0.56}_{-0.31}^{+0.26}$	${0.0124}_{-0.0016}^{+0.0020}$	${0.0510}_{-0.0012}^{+0.0012}$	${1.36}_{-0.19}^{+0.22}$	${1142}_{-43}^{+47}$	${3.9}_{-2.2}^{+2.5}$	${1.5}_{-0.9}^{+1.0}$	${1.5}_{-0.2}^{+0.2}$	$2\times {10}^{-1}$	PC
228798746.01	K2-228 b	${2.69828}_{-0.00022}^{+0.00022}$	${2750.1943}_{-0.0041}^{+0.0039}$	${12.2}_{-2.7}^{+1.3}$	${0.42}_{-0.29}^{+0.30}$	${0.0170}_{-0.0008}^{+0.0013}$	${0.0338}_{-0.0003}^{+0.0003}$	${1.21}_{-0.06}^{+0.10}$	${914}_{-13}^{+14}$	${3.2}_{-1.7}^{+1.7}$	${1.8}_{-1.0}^{+1.0}$	${3.3}_{-1.8}^{+1.2}$	$1\times {10}^{-3}$	VP
228801451.01	K2-229 b	${0.58426}_{-0.00002}^{+0.00002}$	${2750.4691}_{-0.0012}^{+0.0012}$	${3.4}_{-0.6}^{+0.2}$	${0.38}_{-0.26}^{+0.28}$	${0.0133}_{-0.0004}^{+0.0007}$	${0.0131}_{-0.00004}^{+0.00005}$	${1.14}_{-0.03}^{+0.06}$	${1818}_{-15}^{+14}$	${2.7}_{-1.5}^{+1.3}$	${2.2}_{-1.3}^{+1.1}$	${1.5}_{-0.6}^{+0.4}$	$4\times {10}^{-10}$	VP
228801451.02	K2-229 c	${8.32727}_{-0.00043}^{+0.00041}$	${2753.3431}_{-0.0019}^{+0.0019}$	${24.9}_{-5.0}^{+2.0}$	${0.39}_{-0.27}^{+0.29}$	${0.0236}_{-0.0007}^{+0.0015}$	${0.0769}_{-0.0003}^{+0.0003}$	${2.03}_{-0.06}^{+0.12}$	${750}_{-6}^{+6}$	${6.9}_{-2.4}^{+2.3}$	${2.4}_{-0.8}^{+0.8}$	${3.0}_{-1.5}^{+0.8}$	$5\times {10}^{-5}$	VP
228804845.01	K2-230 b	${2.86041}_{-0.00061}^{+0.00061}$	${2749.5918}_{-0.0091}^{+0.0093}$	${7.3}_{-1.6}^{+1.4}$	${0.39}_{-0.26}^{+0.31}$	${0.0129}_{-0.0010}^{+0.0011}$	${0.0409}_{-0.0002}^{+0.0003}$	${1.96}_{-0.16}^{+0.18}$	${1529}_{-22}^{+22}$	${6.5}_{-2.4}^{+2.4}$	${2.7}_{-1.0}^{+1.0}$	${0.6}_{-0.3}^{+0.4}$	$7\times {10}^{-5}$	VP
228809391.01		${19.57833}_{-0.00484}^{+0.00492}$	${2763.8040}_{-0.0076}^{+0.0074}$	${52.5}_{-12.5}^{+5.9}$	${0.42}_{-0.29}^{+0.31}$	${0.0272}_{-0.0016}^{+0.0020}$	${0.1408}_{-0.0015}^{+0.0015}$	${2.77}_{-0.17}^{+0.21}$	${644}_{-10}^{+10}$	${10.1}_{-2.5}^{+2.6}$	${2.4}_{-0.6}^{+0.6}$	${5.1}_{-2.8}^{+1.9}$	$2\times {10}^{-2}$	PC
228809550.01	K2-253 b	${4.00167}_{-0.00013}^{+0.00013}$	${2750.9993}_{-0.0014}^{+0.0013}$	${13.9}_{-2.0}^{+0.8}$	${0.34}_{-0.23}^{+0.26}$	${0.1050}_{-0.0024}^{+0.0046}$	${0.0506}_{-0.0011}^{+0.0010}$	${12.67}_{-0.61}^{+0.69}$	${1238}_{-53}^{+57}$	${70.8}_{-23.2}^{+34.9}$	${27.0}_{-8.8}^{+13.6}$	${2.2}_{-0.8}^{+0.4}$	$3\times {10}^{-4}$	VP
228834632.01		${11.73677}_{-0.00854}^{+0.00795}$	${2758.6048}_{-0.0299}^{+0.0292}$	${35.6}_{-1.7}^{+1.6}$	${0.21}_{-0.15}^{+0.24}$	${0.0270}_{-0.0038}^{+0.0033}$	${0.0875}_{-0.0010}^{+0.0009}$	${1.82}_{-0.26}^{+0.23}$	${516}_{-16}^{+17}$	${5.9}_{-2.7}^{+2.7}$	${2.2}_{-1.0}^{+1.0}$	${4.4}_{-0.6}^{+0.6}$	$2\times {10}^{-2}$	PC
228836835.01		${0.72813}_{-0.00017}^{+0.00020}$	${2750.2622}_{-0.0098}^{+0.0091}$	${7.4}_{-0.9}^{+0.7}$	${0.49}_{-0.33}^{+0.34}$	${0.0273}_{-0.0060}^{+0.0057}$	${0.0121}_{-0.0001}^{+0.0001}$	${1.27}_{-0.28}^{+0.27}$	${932}_{-17}^{+17}$	${3.3}_{-2.5}^{+2.8}$	${4.0}_{-3.0}^{+3.4}$	${10.2}_{-3.2}^{+3.3}$	$4\times {10}^{-2}$	PC
228846243.01		${25.58142}_{-0.01921}^{+0.02417}$	${2756.8674}_{-0.0348}^{+0.0336}$	${22.2}_{-7.3}^{+5.9}$	${0.47}_{-0.31}^{+0.35}$	${0.0406}_{-0.0039}^{+0.0052}$	${0.1931}_{-0.0047}^{+0.0045}$	${8.35}_{-0.93}^{+1.23}$	${914}_{-64}^{+67}$	${41.4}_{-12.0}^{+18.3}$	${6.9}_{-2.0}^{+3.1}$	${0.2}_{-0.2}^{+0.2}$	$9\times {10}^{-2}$	PC
228849382.01	K2-254 b	${4.09639}_{-0.00079}^{+0.00081}$	${2749.9757}_{-0.0106}^{+0.0096}$	${15.8}_{-0.8}^{+0.7}$	${0.72}_{-0.26}^{+0.12}$	${0.0223}_{-0.0032}^{+0.0037}$	${0.0448}_{-0.0005}^{+0.0005}$	${1.63}_{-0.24}^{+0.28}$	${791}_{-26}^{+26}$	${5.2}_{-2.4}^{+2.6}$	${2.6}_{-1.2}^{+1.3}$	${3.2}_{-0.4}^{+0.4}$	$2\times {10}^{-4}$	VP
228849382.02	K2-254 c	${12.11839}_{-0.00321}^{+0.00303}$	${2757.6136}_{-0.0104}^{+0.0101}$	${31.3}_{-8.0}^{+4.8}$	${0.42}_{-0.29}^{+0.33}$	${0.0298}_{-0.0024}^{+0.0032}$	${0.0923}_{-0.0010}^{+0.0010}$	${2.19}_{-0.18}^{+0.24}$	${551}_{-18}^{+18}$	${7.5}_{-2.4}^{+2.5}$	${2.6}_{-0.9}^{+0.9}$	${2.8}_{-1.6}^{+1.5}$	$2\times {10}^{-6}$	VP
228888935.01		${5.69046}_{-0.00028}^{+0.00027}$	${2751.6711}_{-0.0021}^{+0.0020}$	${8.1}_{-0.9}^{+2.5}$	${0.76}_{-0.24}^{+0.06}$	${0.0881}_{-0.0062}^{+0.0032}$	${0.0707}_{-0.0018}^{+0.0017}$	${18.81}_{-1.35}^{+1.20}$	${1503}_{-106}^{+109}$	${115.3}_{-44.1}^{+76.5}$	${32.1}_{-12.4}^{+21.6}$	${0.2}_{-0.1}^{+0.3}$	$1\times {10}^{-1}$	PC
228894622.01	K2-255 b	${1.96417}_{-0.00004}^{+0.00004}$	${2750.3015}_{-0.0008}^{+0.0008}$	${9.1}_{-2.3}^{+0.9}$	${0.44}_{-0.31}^{+0.31}$	${0.0386}_{-0.0013}^{+0.0038}$	${0.0274}_{-0.0003}^{+0.0003}$	${2.90}_{-0.11}^{+0.28}$	${1034}_{-17}^{+17}$	${10.8}_{-2.5}^{+2.6}$	${6.9}_{-1.6}^{+1.7}$	${2.6}_{-1.5}^{+0.9}$	$1\times {10}^{-7}$	VP
228934525.01	K2-154 b	${3.67626}_{-0.00031}^{+0.00030}$	${2752.0533}_{-0.0035}^{+0.0037}$	${14.5}_{-3.9}^{+1.9}$	${0.44}_{-0.30}^{+0.33}$	${0.0288}_{-0.0015}^{+0.0031}$	${0.0405}_{-0.0003}^{+0.0003}$	${1.99}_{-0.11}^{+0.21}$	${715}_{-8}^{+9}$	${6.8}_{-2.4}^{+2.5}$	${3.7}_{-1.3}^{+1.4}$	${3.0}_{-1.8}^{+1.4}$	$5\times {10}^{-10}$	VP
228934525.02	K2-154 c	${7.95486}_{-0.00085}^{+0.00084}$	${2751.3376}_{-0.0043}^{+0.0048}$	${24.9}_{-5.8}^{+2.8}$	${0.42}_{-0.27}^{+0.31}$	${0.0300}_{-0.0019}^{+0.0025}$	${0.0677}_{-0.0005}^{+0.0005}$	${2.07}_{-0.13}^{+0.18}$	${552}_{-7}^{+7}$	${7.0}_{-2.4}^{+2.4}$	${3.0}_{-1.0}^{+1.0}$	${3.3}_{-1.8}^{+1.3}$	$2\times {10}^{-9}$	VP
228964773.01		${37.20364}_{-0.01725}^{+0.01391}$	${2776.7633}_{-0.0115}^{+0.0124}$	${55.7}_{-15.3}^{+9.6}$	${0.42}_{-0.29}^{+0.33}$	${0.0543}_{-0.0046}^{+0.0055}$	${0.2095}_{-0.0021}^{+0.0021}$	${5.10}_{-0.46}^{+0.54}$	${498}_{-10}^{+10}$	${22.0}_{-4.8}^{+6.7}$	${4.6}_{-1.0}^{+1.4}$	${1.7}_{-1.0}^{+1.0}$	$1\times {10}^{-2}$	PC
228968232.01	K2-256 b	${5.52011}_{-0.00289}^{+0.00239}$	${2753.5247}_{-0.0191}^{+0.0202}$	${7.6}_{-1.9}^{+1.3}$	${0.42}_{-0.29}^{+0.34}$	${0.0309}_{-0.0022}^{+0.0028}$	${0.0578}_{-0.0008}^{+0.0008}$	${2.63}_{-0.21}^{+0.25}$	${845}_{-28}^{+28}$	${9.4}_{-2.6}^{+2.7}$	${3.8}_{-1.0}^{+1.1}$	${0.2}_{-0.1}^{+0.1}$	$1\times {10}^{-5}$	VP
228974324.01	K2-257 b	${1.60588}_{-0.00013}^{+0.00014}$	${2750.2875}_{-0.0038}^{+0.0035}$	${8.2}_{-1.8}^{+1.1}$	${0.40}_{-0.27}^{+0.31}$	${0.0153}_{-0.0008}^{+0.0011}$	${0.0216}_{-0.0002}^{+0.0002}$	${0.83}_{-0.05}^{+0.06}$	${789}_{-14}^{+14}$	${0.7}_{-0.4}^{+0.5}$	${0.6}_{-0.4}^{+0.4}$	${2.9}_{-1.5}^{+1.3}$	$7\times {10}^{-11}$	VP
228974907.01		${20.84919}_{-0.03161}^{+0.02660}$	${2759.6108}_{-0.0467}^{+0.0550}$	${33.9}_{-12.5}^{+7.8}$	${0.41}_{-0.29}^{+0.35}$	${0.0103}_{-0.0011}^{+0.0011}$	${0.1828}_{-0.0012}^{+0.0012}$	${3.01}_{-0.32}^{+0.33}$	${1349}_{-49}^{+50}$	${11.1}_{-2.9}^{+3.1}$	${1.7}_{-0.4}^{+0.5}$	${1.2}_{-0.9}^{+1.0}$	$5\times {10}^{-3}$	PC
229004835.01		${16.13655}_{-0.00182}^{+0.00168}$	${2764.6294}_{-0.0035}^{+0.0039}$	${54.6}_{-10.7}^{+4.8}$	${0.38}_{-0.27}^{+0.30}$	${0.0184}_{-0.0007}^{+0.0010}$	${0.1218}_{-0.0005}^{+0.0005}$	${2.02}_{-0.08}^{+0.12}$	${739}_{-7}^{+7}$	${6.8}_{-2.3}^{+2.3}$	${1.8}_{-0.6}^{+0.6}$	${8.4}_{-4.0}^{+2.4}$	$2\times {10}^{-2}$	PC
229017395.01	K2-258 b	${19.09210}_{-0.00633}^{+0.00576}$	${2753.2928}_{-0.0128}^{+0.0147}$	${21.5}_{-4.5}^{+2.0}$	${0.37}_{-0.25}^{+0.32}$	${0.0210}_{-0.0013}^{+0.0014}$	${0.1490}_{-0.0026}^{+0.0025}$	${3.00}_{-0.20}^{+0.21}$	${831}_{-30}^{+30}$	${11.1}_{-2.7}^{+2.6}$	${2.3}_{-0.6}^{+0.6}$	${0.4}_{-0.2}^{+0.1}$	$2\times {10}^{-4}$	VP
229103251.01		${11.67254}_{-0.00402}^{+0.00454}$	${2756.7039}_{-0.0140}^{+0.0131}$	${28.3}_{-9.0}^{+8.6}$	${0.44}_{-0.30}^{+0.36}$	${0.0283}_{-0.0025}^{+0.0033}$	${0.1057}_{-0.0024}^{+0.0023}$	${3.87}_{-0.36}^{+0.47}$	${946}_{-44}^{+43}$	${15.6}_{-3.4}^{+4.2}$	${4.0}_{-0.9}^{+1.1}$	${2.2}_{-1.5}^{+2.7}$	$6\times {10}^{-1}$	PC
229131722.01	K2-259 b	${15.48043}_{-0.00392}^{+0.00332}$	${2752.7094}_{-0.0102}^{+0.0100}$	${29.9}_{-7.1}^{+4.4}$	${0.41}_{-0.28}^{+0.33}$	${0.0189}_{-0.0013}^{+0.0015}$	${0.1271}_{-0.0011}^{+0.0010}$	${2.32}_{-0.17}^{+0.20}$	${795}_{-13}^{+13}$	${8.1}_{-2.5}^{+2.5}$	${1.9}_{-0.6}^{+0.6}$	${1.5}_{-0.8}^{+0.8}$	$2\times {10}^{-3}$	VP
229133720.01		${4.03692}_{-0.00014}^{+0.00013}$	${2750.9634}_{-0.0012}^{+0.0013}$	${13.4}_{-2.3}^{+0.9}$	${0.36}_{-0.25}^{+0.28}$	${0.0285}_{-0.0007}^{+0.0015}$	${0.0456}_{-0.0005}^{+0.0005}$	${2.24}_{-0.07}^{+0.12}$	${870}_{-28}^{+29}$	${7.7}_{-2.3}^{+2.4}$	${3.7}_{-1.1}^{+1.1}$	${2.0}_{-0.9}^{+0.4}$	$5\times {10}^{-8}$	PC

Note. M_P is the mass predicted using the mass–radius relation of Wolfgang et al. (2016) (see Section 6.4). We note that this mass–radius relation was calibrated with sub-Neptunes similar in size to the vast majority of the planets in our validated sample; the predictions may not be accurate for larger candidates, but we report them here anyway for the sake of uniformity. The "Disposition" column indicates the final validation status of each candidate: "VP" = validated planet; "PC" = planet candidate; "FP" = false positive.

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Table 6.  Stellar Parameters

EPIC	${T}_{\mathrm{eff}}$	log g	[Fe/H]	Mass	Radius	Distance	$v\sin i$	Provenance
	(K)	(cgs)	(dex)	(M⊙)	(R⊙)	(pc)	(km s−1)
201092629	${5262}_{-39}^{+43}$	4.54 ± 0.01	$-{0.44}_{-0.03}^{+0.04}$	0.71 ± 0.01	0.75 ± 0.01	${149.6}_{-1.0}^{+1.1}$	2.08 ± 0.29	This work
201102594	${3459}_{-38}^{+65}$	4.89 ± 0.01	$-{0.01}_{-0.18}^{+0.16}$	0.38 ± 0.01	0.37 ± 0.01	109.6 ± 0.6	⋯	⋯
201110617	4597 ± 50	${4.62}_{-0.01}^{+0.02}$	−0.25 ± 0.06	${0.66}_{-0.01}^{+0.02}$	0.66 ± 0.01	150.4 ± 1.0	1.80 ± 0.30	This work
201111557	${5011}_{-239}^{+289}$	4.62 ± 0.01	−0.23 ± 0.23	${0.77}_{-0.03}^{+0.02}$	0.71 ± 0.01	97.5 ± 0.5	⋯	⋯
201127519	${4957}_{-49}^{+47}$	${4.58}_{-0.03}^{+0.02}$	0.03 ± 0.05	0.81 ± 0.03	0.77 ± 0.01	118.0 ± 0.7	1.85 ± 0.22	This work
201128338	${4044}_{-35}^{+34}$	4.67 ± 0.01	${0.12}_{-0.08}^{+0.09}$	0.63 ± 0.01	0.61 ± 0.01	108.7 ± 0.4	⋯	Hirano et al. (2018a)
201132684	${5503}_{-48}^{+51}$	4.45 ± 0.02	0.07 ± 0.07	${0.92}_{-0.02}^{+0.03}$	0.95 ± 0.02	198.2 ± 2.1	⋯	Mayo et al. (2018)
201164625	${6264}_{-81}^{+83}$	3.66 ± 0.03	${0.18}_{-0.03}^{+0.02}$	${1.78}_{-0.03}^{+0.06}$	${3.30}_{-0.16}^{+0.13}$	${1067.1}_{-53.7}^{+36.4}$	11.50 ± 0.46	This work
201166680	${6570}_{-171}^{+269}$	${4.26}_{-0.03}^{+0.02}$	$-{0.03}_{-0.19}^{+0.18}$	${1.29}_{-0.06}^{+0.04}$	1.39 ± 0.03	${269.2}_{-3.4}^{+3.6}$	⋯	⋯
201180665	${6234}_{-258}^{+210}$	${4.29}_{-0.05}^{+0.03}$	${0.02}_{-0.17}^{+0.14}$	${1.17}_{-0.09}^{+0.06}$	1.28 ± 0.03	${611.6}_{-8.8}^{+9.3}$	⋯	⋯
201211526	${5677}_{-39}^{+38}$	4.44 ± 0.02	−0.29 ± 0.03	0.86 ± 0.02	${0.92}_{-0.01}^{+0.02}$	${214.0}_{-2.3}^{+2.4}$	3.69 ± 0.24	This work
201225286	5425 ± 44	${4.56}_{-0.02}^{+0.01}$	−0.07 ± 0.06	${0.90}_{-0.03}^{+0.02}$	0.83 ± 0.01	${171.9}_{-1.3}^{+1.4}$	⋯	Mayo et al. (2018)
201274010	${5636}_{-124}^{+171}$	${4.53}_{-0.02}^{+0.01}$	$-{0.09}_{-0.21}^{+0.17}$	${0.94}_{-0.04}^{+0.03}$	0.88 ± 0.02	${510.3}_{-8.3}^{+8.6}$	⋯	⋯
201352100	${5108}_{-58}^{+61}$	4.60 ± 0.01	−0.08 ± 0.04	${0.83}_{-0.02}^{+0.01}$	0.76 ± 0.01	203.5 ± 3.3	2.15 ± 0.30	This work
201357643	${5793}_{-52}^{+66}$	4.16 ± 0.02	−0.45 ± 0.02	${0.83}_{-0.01}^{+0.02}$	1.25 ± 0.03	${463.4}_{-8.4}^{+9.1}$	4.62 ± 0.24	This work
201386739	${5610}_{-29}^{+32}$	${4.43}_{-0.03}^{+0.04}$	−0.19 ± 0.03	0.87 ± 0.02	0.94 ± 0.03	${723.1}_{-24.7}^{+24.9}$	2.90 ± 0.30	This work
201390048	${4842}_{-45}^{+49}$	4.63 ± 0.01	$-{0.17}_{-0.06}^{+0.05}$	0.75 ± 0.02	0.69 ± 0.01	125.1 ± 0.6	⋯	Mayo et al. (2018)
201390927	${5711}_{-273}^{+285}$	${4.42}_{-0.08}^{+0.06}$	${0.01}_{-0.17}^{+0.15}$	0.97 ± 0.09	${1.01}_{-0.08}^{+0.10}$	${354.8}_{-30.1}^{+34.9}$	⋯	⋯
201392505	${5128}_{-54}^{+53}$	${4.60}_{-0.02}^{+0.01}$	−0.16 ± 0.06	${0.81}_{-0.03}^{+0.02}$	0.75 ± 0.01	${274.3}_{-5.0}^{+5.3}$	2.46 ± 0.29	This work
201437844	${6277}_{-51}^{+52}$	4.25 ± 0.02	−0.22 ± 0.07	${1.08}_{-0.04}^{+0.03}$	1.29 ± 0.02	109.7 ± 0.7	12.90 ± 0.40	Rodriguez et al. (2017)
201595106	5823 ± 19	${4.48}_{-0.02}^{+0.01}$	−0.00 ± 0.03	${1.02}_{-0.02}^{+0.01}$	${0.96}_{-0.01}^{+0.02}$	${233.1}_{-2.4}^{+2.6}$	3.62 ± 0.18	This work
201598502	3845 ± 37	4.73 ± 0.01	−0.09 ± 0.08	0.55 ± 0.01	0.53 ± 0.01	143.6 ± 0.9	⋯	Hirano et al. (2018a)
201615463	${5960}_{-53}^{+52}$	4.09 ± 0.02	0.09 ± 0.06	${1.16}_{-0.03}^{+0.05}$	1.61 ± 0.04	${481.0}_{-8.9}^{+9.7}$	⋯	Mayo et al. (2018)
228707509	${5799}_{-241}^{+197}$	${4.44}_{-0.05}^{+0.04}$	${0.00}_{-0.18}^{+0.16}$	${1.00}_{-0.09}^{+0.06}$	1.00 ± 0.04	${880.7}_{-29.7}^{+32.0}$	⋯	⋯
228720681	${5725}_{-76}^{+73}$	${4.37}_{-0.12}^{+0.13}$	−0.27 ± 0.04	0.88 ± 0.03	${1.02}_{-0.13}^{+0.16}$	${642.5}_{-82.3}^{+102.0}$	12.00 ± 0.60	This work
228721452	${5835}_{-40}^{+38}$	4.48 ± 0.01	0.12 ± 0.06	1.06 ± 0.02	0.99 ± 0.01	201.1 ± 2.5	⋯	Mayo et al. (2018)
228724899	5533 ± 52	4.44 ± 0.02	0.17 ± 0.04	${0.95}_{-0.02}^{+0.03}$	0.97 ± 0.02	${431.5}_{-5.0}^{+5.2}$	2.90 ± 0.30	This work
228725791	${4667}_{-183}^{+305}$	${4.63}_{-0.02}^{+0.01}$	−0.08 ± 0.22	0.74 ± 0.03	${0.69}_{-0.01}^{+0.02}$	260.2 ± 2.1	⋯	⋯
228725972	${5620}_{-45}^{+42}$	${4.55}_{-0.02}^{+0.01}$	−0.19 ± 0.06	0.91 ± 0.02	0.84 ± 0.01	277.7 ± 2.9	⋯	Mayo et al. (2018)
228729473	${4940}_{-41}^{+47}$	3.32 ± 0.04	−0.05 ± 0.02	${1.21}_{-0.14}^{+0.08}$	${3.96}_{-0.11}^{+0.12}$	${579.6}_{-14.6}^{+16.1}$	3.46 ± 0.27	This work
228732031	${5245}_{-52}^{+46}$	4.61 ± 0.01	−0.17 ± 0.03	0.84 ± 0.01	0.75 ± 0.01	${153.7}_{-1.0}^{+1.1}$	4.30 ± 0.20	This work
228734900	${5742}_{-47}^{+49}$	4.08 ± 0.02	0.38 ± 0.06	${1.27}_{-0.04}^{+0.02}$	1.70 ± 0.04	${360.3}_{-5.7}^{+5.9}$	⋯	Mayo et al. (2018)
228735255	${5705}_{-48}^{+50}$	4.45 ± 0.01	0.13 ± 0.04	1.00 ± 0.02	0.99 ± 0.01	${341.6}_{-5.1}^{+5.5}$	3.80 ± 0.20	Giles et al. 2017
228736155	${5424}_{-46}^{+48}$	4.47 ± 0.03	−0.03 ± 0.07	0.88 ± 0.03	0.91 ± 0.02	${211.2}_{-3.1}^{+3.4}$	⋯	Mayo et al. (2018)
228739306	${5528}_{-86}^{+97}$	4.45 ± 0.03	−0.10 ± 0.04	${0.88}_{-0.03}^{+0.04}$	0.92 ± 0.02	410.5 ± 4.9	2.60 ± 0.20	This work
228748383	${6504}_{-419}^{+329}$	${4.16}_{-0.06}^{+0.05}$	${0.04}_{-0.16}^{+0.14}$	${1.32}_{-0.12}^{+0.09}$	1.57 ± 0.06	${528.3}_{-14.7}^{+16.9}$	⋯	⋯
228748826	${5172}_{-44}^{+46}$	4.53 ± 0.03	−0.09 ± 0.04	${0.80}_{-0.02}^{+0.03}$	0.81 ± 0.02	${417.6}_{-6.0}^{+6.2}$	2.20 ± 0.30	This work
228753871	${5312}_{-156}^{+190}$	${4.59}_{-0.02}^{+0.01}$	$-{0.18}_{-0.19}^{+0.16}$	${0.84}_{-0.03}^{+0.02}$	0.77 ± 0.01	295.9 ± 2.0	⋯	⋯
228758778	${3717}_{-50}^{+85}$	4.76 ± 0.01	$-{0.04}_{-0.19}^{+0.18}$	0.52 ± 0.01	0.49 ± 0.01	147.7 ± 1.0	⋯	⋯
228758948	${5931}_{-45}^{+42}$	${4.45}_{-0.02}^{+0.01}$	0.11 ± 0.03	1.09 ± 0.02	1.03 ± 0.02	${446.2}_{-7.0}^{+7.5}$	4.40 ± 0.20	This work
228763938	${5152}_{-39}^{+41}$	${4.50}_{-0.01}^{+0.02}$	−0.09 ± 0.04	${0.79}_{-0.01}^{+0.02}$	0.82 ± 0.01	${229.9}_{-1.9}^{+2.1}$	2.20 ± 0.20	This work
228784812	${5815}_{-238}^{+187}$	${4.43}_{-0.05}^{+0.03}$	${0.01}_{-0.19}^{+0.15}$	${1.01}_{-0.09}^{+0.06}$	${1.01}_{-0.02}^{+0.03}$	${345.4}_{-5.0}^{+4.9}$	⋯	⋯
228798746	${4715}_{-46}^{+48}$	4.66 ± 0.01	−0.25 ± 0.06	0.71 ± 0.02	0.65 ± 0.01	142.4 ± 3.2	⋯	Mayo et al. (2018)
228801451	${5315}_{-31}^{+35}$	${4.59}_{-0.01}^{+0.00}$	−0.09 ± 0.02	0.87 ± 0.01	0.79 ± 0.01	103.8 ± 1.0	2.46 ± 0.22	This work
228804845	${5945}_{-25}^{+23}$	4.20 ± 0.02	0.10 ± 0.04	1.11 ± 0.02	1.39 ± 0.04	${548.9}_{-13.5}^{+14.3}$	5.20 ± 0.20	This work
228809391	${5674}_{-77}^{+63}$	${4.49}_{-0.03}^{+0.02}$	−0.01 ± 0.03	0.97 ± 0.03	0.93 ± 0.02	${333.7}_{-4.7}^{+4.8}$	3.20 ± 0.20	This work
228809550	${6027}_{-240}^{+221}$	${4.39}_{-0.05}^{+0.03}$	$-{0.00}_{-0.19}^{+0.17}$	${1.08}_{-0.08}^{+0.05}$	1.10 ± 0.04	${901.8}_{-27.9}^{+30.0}$	⋯	⋯
228834632	${4395}_{-125}^{+135}$	4.67 ± 0.01	$-{0.21}_{-0.18}^{+0.17}$	0.65 ± 0.02	0.62 ± 0.01	285.3 ± 3.0	⋯	⋯
228836835	${3562}_{-35}^{+70}$	4.83 ± 0.01	$-{0.01}_{-0.18}^{+0.16}$	0.45 ± 0.01	0.43 ± 0.01	${150.8}_{-1.7}^{+1.8}$	⋯	⋯
228846243	${6644}_{-454}^{+413}$	${4.05}_{-0.06}^{+0.05}$	${0.06}_{-0.15}^{+0.14}$	${1.47}_{-0.11}^{+0.10}$	${1.89}_{-0.10}^{+0.11}$	${1405.4}_{-70.8}^{+77.3}$	⋯	⋯
228849382	${4629}_{-123}^{+168}$	4.64 ± 0.01	$-{0.14}_{-0.15}^{+0.18}$	${0.71}_{-0.03}^{+0.02}$	0.67 ± 0.01	229.4 ± 1.3	⋯	⋯
228888935	${6452}_{-413}^{+452}$	4.01 ± 0.05	${0.08}_{-0.14}^{+0.13}$	1.45 ± 0.11	1.97 ± 0.09	${1278.0}_{-46.9}^{+50.4}$	⋯	⋯
228894622	${4676}_{-61}^{+63}$	4.62 ± 0.02	$-{0.14}_{-0.06}^{+0.07}$	0.71 ± 0.03	0.69 ± 0.01	192.4 ± 1.5	2.46 ± 0.27	This work
228934525	${4097}_{-45}^{+40}$	4.65 ± 0.01	${0.21}_{-0.10}^{+0.09}$	${0.65}_{-0.01}^{+0.02}$	0.63 ± 0.01	129.8 ± 0.4	⋯	Hirano et al. (2018a)
228964773	${5574}_{-61}^{+64}$	${4.52}_{-0.04}^{+0.03}$	−0.18 ± 0.03	0.89 ± 0.03	${0.86}_{-0.02}^{+0.03}$	${802.5}_{-20.6}^{+25.3}$	3.40 ± 0.20	This work
228968232	${5219}_{-136}^{+179}$	${4.58}_{-0.02}^{+0.01}$	−0.10 ± 0.17	${0.84}_{-0.04}^{+0.03}$	0.78 ± 0.02	${580.5}_{-13.9}^{+14.9}$	⋯	⋯
228974324	${3725}_{-46}^{+80}$	4.76 ± 0.01	$-{0.03}_{-0.18}^{+0.17}$	0.52 ± 0.01	0.50 ± 0.01	64.1 ± 0.3	⋯	⋯
228974907	${8003}_{-187}^{+370}$	3.86 ± 0.03	$-{0.32}_{-0.14}^{+0.11}$	${1.87}_{-0.05}^{+0.02}$	${2.67}_{-0.11}^{+0.08}$	${379.9}_{-11.2}^{+10.7}$	⋯	⋯
229004835	${5831}_{-35}^{+38}$	4.40 ± 0.02	−0.22 ± 0.01	0.92 ± 0.01	1.00 ± 0.01	${122.4}_{-0.9}^{+0.8}$	3.77 ± 0.12	This work
229017395	${6351}_{-228}^{+198}$	${4.29}_{-0.04}^{+0.03}$	${0.01}_{-0.17}^{+0.15}$	${1.21}_{-0.08}^{+0.05}$	1.31 ± 0.03	${675.2}_{-11.5}^{+11.6}$	⋯	⋯
229103251	${6220}_{-305}^{+225}$	${4.30}_{-0.05}^{+0.03}$	${0.02}_{-0.18}^{+0.15}$	${1.16}_{-0.10}^{+0.07}$	${1.26}_{-0.03}^{+0.04}$	${756.2}_{-14.1}^{+15.0}$	⋯	⋯
229131722	${6059}_{-76}^{+62}$	${4.39}_{-0.03}^{+0.02}$	0.16 ± 0.04	1.14 ± 0.03	${1.13}_{-0.02}^{+0.03}$	${422.1}_{-7.8}^{+7.7}$	5.23 ± 0.20	This work
229133720	${4964}_{-139}^{+170}$	${4.61}_{-0.02}^{+0.01}$	$-{0.17}_{-0.16}^{+0.17}$	${0.78}_{-0.03}^{+0.02}$	0.72 ± 0.01	105.2 ± 0.5	⋯	⋯

Note. "Provenance" indicates the source of the spectroscopic parameters used as priors in our analysis (see Section 4.4). The $v\sin i$ uncertainties are internal to the Kea pipeline and do not account for other types of line broadening; thus they are likely to be underestimated.

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Table 7.  Individual False Positive Scenario Likelihoods Computed by vespa

EPIC	L_beba	L_beb_P × 2a	L_ebb	L_eb_P × 2b	L_hebc	L_heb_P × 2c	L_pld	FPP
201092629.01	0	0	$1.1\times {10}^{-11}$	$7.8\times {10}^{-10}$	$5.7\times {10}^{-52}$	$1.4\times {10}^{-20}$	$1.2\times {10}^{-2}$	$6.8\times {10}^{-8}$
201102594.01	0	0	$1.0\times {10}^{-22}$	$1.1\times {10}^{-13}$	$7.6\times {10}^{-30}$	$2.9\times {10}^{-21}$	$1.8\times {10}^{-2}$	$5.9\times {10}^{-12}$
201110617.01	0	0	$2.3\times {10}^{-52}$	$4.5\times {10}^{-13}$	$1.1\times {10}^{-90}$	$3.7\times {10}^{-42}$	$2.3\times {10}^{-1}$	$2.0\times {10}^{-12}$
201111557.01	0	0	$6.1\times {10}^{-9}$	$1.2\times {10}^{-6}$	$1.0\times {10}^{-32}$	$2.4\times {10}^{-14}$	$4.0\times {10}^{-3}$	$3.0\times {10}^{-4}$
201127519.01	0	0	$1.1\times {10}^{-3}$	$3.2\times {10}^{-6}$	$2.2\times {10}^{-86}$	$4.6\times {10}^{-27}$	$2.8\times {10}^{-2}$	$3.9\times {10}^{-2}$
201128338.01	0	0	$3.0\times {10}^{-16}$	$2.0\times {10}^{-10}$	$3.0\times {10}^{-12}$	$1.1\times {10}^{-12}$	$1.6\times {10}^{-3}$	$1.3\times {10}^{-7}$
201132684.01	0	0	$2.1\times {10}^{-9}$	$5.6\times {10}^{-8}$	$1.2\times {10}^{-49}$	$1.4\times {10}^{-18}$	$2.9\times {10}^{-2}$	$2.0\times {10}^{-6}$
201132684.02	0	0	$4.7\times {10}^{-14}$	$3.4\times {10}^{-9}$	$4.4\times {10}^{-25}$	$2.3\times {10}^{-12}$	$4.7\times {10}^{-3}$	$7.2\times {10}^{-7}$
201164625.01	0	0	$4.6\times {10}^{-6}$	$3.0\times {10}^{-7}$	$1.5\times {10}^{-6}$	$5.0\times {10}^{-7}$	$1.9\times {10}^{-3}$	$3.6\times {10}^{-3}$
201166680.02	$1.0\times {10}^{-5}$	$3.3\times {10}^{-6}$	$5.5\times {10}^{-6}$	$2.3\times {10}^{-6}$	$1.5\times {10}^{-30}$	$2.8\times {10}^{-16}$	$9.7\times {10}^{-3}$	$2.2\times {10}^{-3}$
201166680.03	$3.2\times {10}^{-6}$	$1.5\times {10}^{-6}$	$2.0\times {10}^{-6}$	$9.0\times {10}^{-8}$	$5.8\times {10}^{-20}$	$5.8\times {10}^{-13}$	$1.9\times {10}^{-3}$	$3.6\times {10}^{-3}$
201180665.01	0	0	$8.6\times {10}^{-4}$	$1.7\times {10}^{-6}$	$1.2\times {10}^{-6}$	$1.6\times {10}^{-8}$	$4.9\times {10}^{-4}$	$6.4\times {10}^{-1}$
201211526.01	0	0	$3.4\times {10}^{-7}$	$3.6\times {10}^{-6}$	$3.9\times {10}^{-25}$	$3.2\times {10}^{-12}$	$5.9\times {10}^{-3}$	$6.7\times {10}^{-4}$
201225286.01	0	0	$2.2\times {10}^{-6}$	$2.1\times {10}^{-6}$	$1.7\times {10}^{-44}$	$1.8\times {10}^{-13}$	$2.2\times {10}^{-2}$	$1.9\times {10}^{-4}$
201274010.01	$1.6\times {10}^{-4}$	$2.8\times {10}^{-4}$	$1.3\times {10}^{-5}$	$1.6\times {10}^{-5}$	$1.7\times {10}^{-17}$	$2.7\times {10}^{-10}$	$4.8\times {10}^{-3}$	$8.9\times {10}^{-2}$
201352100.01	0	0	$9.1\times {10}^{-6}$	$3.1\times {10}^{-5}$	$2.7\times {10}^{-79}$	$8.2\times {10}^{-22}$	$2.6\times {10}^{-2}$	$1.5\times {10}^{-3}$
201357643.01	0	0	$2.7\times {10}^{-6}$	$4.4\times {10}^{-6}$	$1.8\times {10}^{-89}$	$4.4\times {10}^{-24}$	$3.2\times {10}^{-2}$	$2.2\times {10}^{-4}$
201386739.01	0	0	$1.5\times {10}^{-12}$	$1.8\times {10}^{-7}$	$1.9\times {10}^{-122}$	$5.9\times {10}^{-29}$	$3.2\times {10}^{-3}$	$5.7\times {10}^{-5}$
201390048.01	$4.6\times {10}^{-5}$	$5.8\times {10}^{-6}$	$2.3\times {10}^{-16}$	$8.5\times {10}^{-9}$	$1.9\times {10}^{-96}$	$2.1\times {10}^{-24}$	$2.2\times {10}^{-2}$	$2.3\times {10}^{-3}$
201390927.01	0	0	$1.2\times {10}^{-10}$	$4.2\times {10}^{-8}$	$1.2\times {10}^{-12}$	$1.6\times {10}^{-9}$	$1.7\times {10}^{-3}$	$2.6\times {10}^{-5}$
201392505.01	0	0	$3.0\times {10}^{-18}$	$1.2\times {10}^{-11}$	$1.7\times {10}^{-126}$	$1.2\times {10}^{-38}$	$1.7\times {10}^{-4}$	$7.0\times {10}^{-8}$
201437844.01	0	0	$2.0\times {10}^{-7}$	$1.7\times {10}^{-5}$	$9.6\times {10}^{-71}$	$5.1\times {10}^{-20}$	$1.9\times {10}^{-3}$	$8.7\times {10}^{-3}$
201437844.02	0	0	$1.7\times {10}^{-6}$	$1.4\times {10}^{-7}$	$2.5\times {10}^{-76}$	$2.5\times {10}^{-34}$	$1.8\times {10}^{-3}$	$1.0\times {10}^{-3}$
201595106.01	0	0	$9.6\times {10}^{-5}$	$3.9\times {10}^{-4}$	$5.3\times {10}^{-20}$	$2.9\times {10}^{-12}$	$2.2\times {10}^{-1}$	$2.2\times {10}^{-3}$
201598502.01	0	0	$2.0\times {10}^{-11}$	$4.8\times {10}^{-7}$	$1.9\times {10}^{-17}$	$3.7\times {10}^{-10}$	$1.0\times {10}^{-2}$	$4.7\times {10}^{-5}$
201615463.01	$4.0\times {10}^{-7}$	$1.3\times {10}^{-6}$	$4.1\times {10}^{-9}$	$6.1\times {10}^{-9}$	$5.8\times {10}^{-16}$	$6.0\times {10}^{-10}$	$4.9\times {10}^{-3}$	$3.4\times {10}^{-4}$
228707509.01	0	0	$8.0\times {10}^{-6}$	$1.3\times {10}^{-7}$	$1.8\times {10}^{-15}$	$6.0\times {10}^{-19}$	$1.1\times {10}^{-2}$	$7.4\times {10}^{-4}$
228720681.01	0	0	$1.9\times {10}^{-4}$	$1.2\times {10}^{-6}$	$8.6\times {10}^{-6}$	$1.2\times {10}^{-10}$	$2.0\times {10}^{-2}$	$1.0\times {10}^{-2}$
228721452.01	0	0	$2.5\times {10}^{-5}$	$2.7\times {10}^{-4}$	$2.2\times {10}^{-26}$	$9.2\times {10}^{-22}$	$8.8\times {10}^{-2}$	$3.3\times {10}^{-3}$
228721452.02	0	0	$7.1\times {10}^{-17}$	$3.8\times {10}^{-7}$	$8.9\times {10}^{-155}$	$4.6\times {10}^{-23}$	$9.4\times {10}^{-3}$	$4.1\times {10}^{-5}$
228724899.01	0	0	$1.7\times {10}^{-3}$	$1.7\times {10}^{-4}$	$2.4\times {10}^{-10}$	$6.3\times {10}^{-7}$	$1.1\times {10}^{-2}$	$1.4\times {10}^{-1}$
228725791.01	0	0	$4.1\times {10}^{-14}$	$1.9\times {10}^{-9}$	$1.7\times {10}^{-17}$	$5.1\times {10}^{-13}$	$4.7\times {10}^{-2}$	$4.0\times {10}^{-8}$
228725791.02	0	0	$1.3\times {10}^{-9}$	$4.7\times {10}^{-8}$	$1.5\times {10}^{-14}$	$1.7\times {10}^{-10}$	$1.3\times {10}^{-2}$	$3.7\times {10}^{-6}$
228725972.01	0	0	$1.7\times {10}^{-10}$	$8.4\times {10}^{-7}$	$5.3\times {10}^{-58}$	$9.1\times {10}^{-15}$	$1.7\times {10}^{-2}$	$5.0\times {10}^{-5}$
228725972.02	0	0	$4.2\times {10}^{-10}$	$1.7\times {10}^{-6}$	$8.6\times {10}^{-70}$	$4.4\times {10}^{-25}$	$7.6\times {10}^{-3}$	$2.2\times {10}^{-4}$
228729473.01	0	0	$2.3\times {10}^{-3}$	$1.3\times {10}^{-6}$	$2.7\times {10}^{-77}$	$3.3\times {10}^{-28}$	$8.0\times {10}^{-3}$	$2.2\times {10}^{-1}$
228732031.01	0	0	$6.5\times {10}^{-43}$	$1.2\times {10}^{-8}$	$9.9\times {10}^{-62}$	$1.8\times {10}^{-49}$	$7.5\times {10}^{0}$	$1.6\times {10}^{-9}$
228734900.01	$6.7\times {10}^{-6}$	$4.7\times {10}^{-6}$	$1.4\times {10}^{-8}$	$2.6\times {10}^{-7}$	$6.1\times {10}^{-15}$	$1.8\times {10}^{-10}$	$3.3\times {10}^{-3}$	$3.5\times {10}^{-3}$
228735255.01	0	0	$2.1\times {10}^{-21}$	$1.4\times {10}^{-16}$	$2.6\times {10}^{-58}$	$7.2\times {10}^{-31}$	$1.5\times {10}^{-2}$	$9.5\times {10}^{-15}$
228736155.01	0	0	$6.2\times {10}^{-15}$	$8.0\times {10}^{-9}$	$2.3\times {10}^{-33}$	$1.7\times {10}^{-12}$	$4.5\times {10}^{-2}$	$1.8\times {10}^{-7}$
228739306.01	0	0	$5.1\times {10}^{-9}$	$2.5\times {10}^{-6}$	$6.6\times {10}^{-42}$	$2.1\times {10}^{-17}$	$4.4\times {10}^{-2}$	$5.6\times {10}^{-5}$
228748383.01	0	0	$2.3\times {10}^{-7}$	$9.9\times {10}^{-9}$	$2.1\times {10}^{-12}$	$6.3\times {10}^{-12}$	$1.9\times {10}^{-3}$	$1.3\times {10}^{-4}$
228748826.01	0	0	$1.2\times {10}^{-12}$	$2.5\times {10}^{-6}$	$5.2\times {10}^{-45}$	$7.9\times {10}^{-19}$	$8.8\times {10}^{-2}$	$2.8\times {10}^{-5}$
228753871.01	$2.5\times {10}^{-5}$	$2.7\times {10}^{-5}$	$4.8\times {10}^{-5}$	$5.0\times {10}^{-6}$	$1.6\times {10}^{-15}$	$3.7\times {10}^{-10}$	$1.4\times {10}^{-3}$	$7.0\times {10}^{-2}$
228758778.01	0	0	$1.4\times {10}^{-17}$	$1.3\times {10}^{-9}$	$1.9\times {10}^{-14}$	$3.3\times {10}^{-13}$	$3.2\times {10}^{-3}$	$4.1\times {10}^{-7}$
228758948.01	0	0	$5.1\times {10}^{-7}$	$9.1\times {10}^{-6}$	$8.1\times {10}^{-82}$	$1.6\times {10}^{-24}$	$2.4\times {10}^{-2}$	$4.1\times {10}^{-4}$
228763938.01	0	0	$1.7\times {10}^{-9}$	$1.7\times {10}^{-7}$	$9.6\times {10}^{-28}$	$5.6\times {10}^{-13}$	$4.0\times {10}^{-3}$	$4.5\times {10}^{-5}$
228784812.01	$6.0\times {10}^{-4}$	$1.4\times {10}^{-3}$	$2.5\times {10}^{-4}$	$1.7\times {10}^{-4}$	$1.8\times {10}^{-5}$	$1.0\times {10}^{-5}$	$9.9\times {10}^{-3}$	$2.0\times {10}^{-1}$
228798746.01	$2.3\times {10}^{-4}$	$5.7\times {10}^{-6}$	$2.9\times {10}^{-12}$	$4.4\times {10}^{-7}$	$7.7\times {10}^{-224}$	$3.7\times {10}^{-39}$	$1.7\times {10}^{-1}$	$1.4\times {10}^{-3}$
228801451.01	0	0	$8.1\times {10}^{-18}$	$1.7\times {10}^{-9}$	$1.2\times {10}^{-218}$	$1.4\times {10}^{-102}$	$1.8\times {10}^{-1}$	$9.4\times {10}^{-9}$
228801451.02	0	0	$1.9\times {10}^{-8}$	$2.7\times {10}^{-5}$	$3.5\times {10}^{-141}$	$2.0\times {10}^{-16}$	$2.1\times {10}^{-2}$	$1.3\times {10}^{-3}$
228804845.01	0	0	$1.6\times {10}^{-7}$	$7.8\times {10}^{-7}$	$2.7\times {10}^{-17}$	$2.2\times {10}^{-11}$	$1.3\times {10}^{-2}$	$7.2\times {10}^{-5}$
228809391.01	0	0	$4.5\times {10}^{-5}$	$1.3\times {10}^{-6}$	$9.4\times {10}^{-24}$	$4.6\times {10}^{-14}$	$2.8\times {10}^{-3}$	$1.6\times {10}^{-2}$
228809550.01	0	0	$1.2\times {10}^{-5}$	$2.9\times {10}^{-6}$	$1.7\times {10}^{-11}$	$7.1\times {10}^{-8}$	$5.1\times {10}^{-2}$	$3.0\times {10}^{-4}$
228834632.01	$2.2\times {10}^{-5}$	$5.1\times {10}^{-5}$	$7.6\times {10}^{-10}$	$3.7\times {10}^{-8}$	$3.8\times {10}^{-28}$	$2.1\times {10}^{-13}$	$3.3\times {10}^{-3}$	$2.2\times {10}^{-2}$
228836835.01	$2.7\times {10}^{-4}$	$1.4\times {10}^{-3}$	$2.5\times {10}^{-5}$	$1.8\times {10}^{-4}$	$1.6\times {10}^{-7}$	$2.6\times {10}^{-6}$	$4.2\times {10}^{-2}$	$4.3\times {10}^{-2}$
228846243.01	0	0	$4.4\times {10}^{-5}$	$3.6\times {10}^{-5}$	$8.3\times {10}^{-7}$	$1.3\times {10}^{-6}$	$8.7\times {10}^{-4}$	$8.6\times {10}^{-2}$
228849382.01	0	0	$1.4\times {10}^{-5}$	$4.9\times {10}^{-5}$	$6.3\times {10}^{-12}$	$5.8\times {10}^{-8}$	$1.1\times {10}^{-2}$	$6.0\times {10}^{-3}$
228849382.02	0	0	$1.9\times {10}^{-9}$	$1.4\times {10}^{-7}$	$2.3\times {10}^{-33}$	$1.6\times {10}^{-13}$	$3.6\times {10}^{-3}$	$3.9\times {10}^{-5}$
228888935.01	0	0	$2.9\times {10}^{-3}$	$1.1\times {10}^{-5}$	$1.9\times {10}^{-5}$	$4.2\times {10}^{-7}$	$1.9\times {10}^{-2}$	$1.3\times {10}^{-1}$
228894622.01	0	0	$8.8\times {10}^{-13}$	$2.6\times {10}^{-8}$	$3.1\times {10}^{-50}$	$5.6\times {10}^{-24}$	$2.2\times {10}^{-1}$	$1.2\times {10}^{-7}$
228934525.01	0	0	$1.1\times {10}^{-16}$	$9.8\times {10}^{-10}$	$8.6\times {10}^{-17}$	$5.5\times {10}^{-10}$	$1.3\times {10}^{-1}$	$1.2\times {10}^{-8}$
228934525.02	0	0	$1.6\times {10}^{-25}$	$2.1\times {10}^{-14}$	$8.0\times {10}^{-21}$	$5.1\times {10}^{-11}$	$9.2\times {10}^{-4}$	$5.5\times {10}^{-8}$
228964773.01	0	0	$3.2\times {10}^{-6}$	$7.6\times {10}^{-6}$	$1.6\times {10}^{-23}$	$6.6\times {10}^{-12}$	$7.5\times {10}^{-4}$	$1.4\times {10}^{-2}$
228968232.01	0	0	$2.3\times {10}^{-31}$	$1.8\times {10}^{-9}$	$3.1\times {10}^{-132}$	$1.6\times {10}^{-33}$	$1.7\times {10}^{-4}$	$1.0\times {10}^{-5}$
228974324.01	0	0	$9.4\times {10}^{-114}$	$5.0\times {10}^{-12}$	$1.0\times {10}^{-90}$	$2.3\times {10}^{-24}$	$7.6\times {10}^{-2}$	$6.6\times {10}^{-11}$
228974907.01	0	0	$5.8\times {10}^{-6}$	$2.4\times {10}^{-7}$	$2.3\times {10}^{-6}$	$9.7\times {10}^{-7}$	$1.7\times {10}^{-3}$	$5.5\times {10}^{-3}$
229004835.01	0	0	$2.4\times {10}^{-4}$	$1.8\times {10}^{-6}$	$3.3\times {10}^{-16}$	$6.0\times {10}^{-9}$	$1.1\times {10}^{-2}$	$2.2\times {10}^{-2}$
229017395.01	0	0	$2.0\times {10}^{-8}$	$6.2\times {10}^{-8}$	$4.3\times {10}^{-18}$	$5.1\times {10}^{-12}$	$5.3\times {10}^{-4}$	$1.5\times {10}^{-4}$
229103251.01	0	0	$4.6\times {10}^{-4}$	$1.9\times {10}^{-4}$	$4.5\times {10}^{-6}$	$4.3\times {10}^{-6}$	$4.4\times {10}^{-4}$	$6.0\times {10}^{-1}$
229131722.01	0	0	$5.7\times {10}^{-6}$	$1.6\times {10}^{-6}$	$1.1\times {10}^{-33}$	$3.1\times {10}^{-14}$	$3.2\times {10}^{-3}$	$2.2\times {10}^{-3}$
229133720.01	0	0	$1.3\times {10}^{-19}$	$2.2\times {10}^{-8}$	$1.8\times {10}^{-121}$	$3.9\times {10}^{-25}$	$4.3\times {10}^{-1}$	$5.1\times {10}^{-8}$

Notes.

^aLikelihood that the signal is due to a background eclipsing binary, at the measured period or twice that. ^bLikelihood that the signal is due to an eclipsing binary, at the measured period or twice that. ^cLikelihood that the signal is due to a hierarchical star system with an eclipsing component, at the measured period or twice that. ^dLikelihood that the signal is due to a planet.

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Table 8.  Additional Constraints to vespa

EPIC	Maxrad (arcsec)	Secthresh
201092629.01	20.7	$1\times {10}^{-4}$
201102594.01	15.1	$2\times {10}^{-4}$
201110617.01	15.9	$1\times {10}^{-4}$
201111557.01	17.5	$1\times {10}^{-4}$
201127519.01	10.3	$3\times {10}^{-3}$
201128338.01	18.3	$2\times {10}^{-4}$
201132684.01	21.5	$3\times {10}^{-4}$
201132684.02	21.5	$2\times {10}^{-4}$
201164625.01	19.1	$1\times {10}^{-5}$
201166680.02	22.3	$5\times {10}^{-5}$
201166680.03	22.3	$1\times {10}^{-4}$
201180665.01	8.8	$2\times {10}^{-4}$
201211526.01	13.5	$8\times {10}^{-5}$
201225286.01	12.7	$2\times {10}^{-4}$
201274010.01	16.7	$2\times {10}^{-4}$
201352100.01	10.3	$1\times {10}^{-4}$
201357643.01	6.4	$1\times {10}^{-4}$
201386739.01	16.7	$3\times {10}^{-4}$
201390048.01	10.3	$2\times {10}^{-4}$
201390927.01	14.3	$2\times {10}^{-4}$
201392505.01	8.0	$1\times {10}^{-3}$
201437844.01	31.8	$8\times {10}^{-4}$
201437844.02	31.8	$2\times {10}^{-4}$
201595106.01	17.5	$2\times {10}^{-4}$
201598502.01	15.1	$3\times {10}^{-4}$
201615463.01	16.7	$3\times {10}^{-4}$
228707509.01	14.3	$3\times {10}^{-4}$
228720681.01	10.3	$5\times {10}^{-4}$
228721452.01	14.3	$5\times {10}^{-5}$
228721452.02	14.3	$5\times {10}^{-5}$
228724899.01	11.1	$1\times {10}^{-4}$
228725791.01	11.9	$5\times {10}^{-4}$
228725791.02	11.9	$5\times {10}^{-4}$
228725972.01	14.3	$2\times {10}^{-4}$
228725972.02	14.3	$2\times {10}^{-4}$
228729473.01	19.1	$2\times {10}^{-4}$
228732031.01	21.5	$1\times {10}^{-4}$
228734900.01	15.9	$6\times {10}^{-4}$
228735255.01	16.7	$1\times {10}^{-4}$
228736155.01	15.1	$1\times {10}^{-4}$
228739306.01	15.1	$1\times {10}^{-4}$
228748383.01	15.9	$2\times {10}^{-4}$
228748826.01	15.1	$2\times {10}^{-4}$
228753871.01	13.5	$1\times {10}^{-4}$
228758778.01	12.7	$8\times {10}^{-4}$
228758948.01	17.5	$2\times {10}^{-4}$
228763938.01	14.3	$1\times {10}^{-4}$
228784812.01	8.8	$5\times {10}^{-5}$
228798746.01	9.6	$1\times {10}^{-4}$
228801451.01	18.3	$1\times {10}^{-4}$
228801451.02	18.3	$2\times {10}^{-4}$
228804845.01	19.1	$1\times {10}^{-4}$
228809391.01	9.6	$1\times {10}^{-4}$
228809550.01	11.1	$3\times {10}^{-4}$
228834632.01	11.9	$2\times {10}^{-4}$
228836835.01	8.0	$1\times {10}^{-4}$
228846243.01	9.6	$5\times {10}^{-4}$
228849382.01	8.0	$3\times {10}^{-4}$
228849382.02	8.0	$5\times {10}^{-4}$
228888935.01	8.8	$2\times {10}^{-3}$
228894622.01	12.7	$2\times {10}^{-4}$
228934525.01	9.6	$2\times {10}^{-4}$
228934525.02	9.6	$5\times {10}^{-4}$
228964773.01	7.2	$8\times {10}^{-4}$
228968232.01	10.3	$5\times {10}^{-4}$
228974324.01	11.9	$1\times {10}^{-4}$
228974907.01	32.6	$3\times {10}^{-5}$
229004835.01	11.1	$3\times {10}^{-5}$
229017395.01	15.9	$2\times {10}^{-4}$
229103251.01	16.7	$1\times {10}^{-4}$
229131722.01	12.7	$8\times {10}^{-5}$
229133720.01	18.3	$2\times {10}^{-4}$

Notes. The columns "maxrad" and "secthresh" refer to the maximum radius (the angular size of the photometric aperture) and the secondary eclipse threshold (the maximum secondary eclipse depth allowed by the light curve), respectively.

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Table 9.  WIYN/NESSI Data Sets Used in This Work

EPIC	Filter Center	Filter Width	Obs. Date
	(nm)	(nm)
201092629	562 nm	44 nm	2017 May 15
201092629	832 nm	40 nm	2017 May 15
201092629	562 nm	44 nm	2017 Mar 18
201092629	832 nm	40 nm	2017 Mar 18
201102594	562 nm	44 nm	2017 Apr 05
201102594	832 nm	40 nm	2017 Apr 05
201110617	832 nm	40 nm	2017 Mar 10
201110617	562 nm	44 nm	2017 Mar 10
201111557	562 nm	44 nm	2017 Mar 15
201111557	832 nm	40 nm	2017 Mar 15
201127519	562 nm	44 nm	2017 Mar 11
201127519	832 nm	40 nm	2017 Mar 11
201128338	832 nm	40 nm	2017 Mar 10
201128338	562 nm	44 nm	2017 Mar 10
201132684	832 nm	40 nm	2017 May 12
201132684	562 nm	44 nm	2017 May 12
201132684	562 nm	44 nm	2017 Mar 15
201132684	832 nm	40 nm	2017 Mar 15
201164625	562 nm	44 nm	2017 Mar 18
201164625	832 nm	40 nm	2017 Mar 18
201164625	562 nm	44 nm	2017 May 12
201164625	832 nm	40 nm	2017 May 12
201180665	832 nm	40 nm	2017 Mar 18
201180665	562 nm	44 nm	2017 Mar 18
201211526	832 nm	40 nm	2017 Mar 18
201211526	562 nm	44 nm	2017 Mar 18
201225286	562 nm	44 nm	2017 Apr 03
201225286	832 nm	40 nm	2017 Apr 03
201352100	562 nm	44 nm	2017 Mar 15
201352100	832 nm	40 nm	2017 Mar 15
201357643	562 nm	44 nm	2017 Mar 18
201357643	832 nm	40 nm	2017 Mar 18
201386739	562 nm	44 nm	2017 Mar 17
201386739	832 nm	40 nm	2017 Mar 17
201390927	832 nm	40 nm	2017 Mar 17
201390927	562 nm	44 nm	2017 Mar 17
201392505	832 nm	40 nm	2017 Mar 18
201392505	562 nm	44 nm	2017 Mar 18
201437844	562 nm	44 nm	2017 Mar 11
201437844	832 nm	40 nm	2017 Mar 11
201595106	832 nm	40 nm	2017 Mar 18
201595106	562 nm	44 nm	2017 Mar 18
201598502	832 nm	40 nm	2017 Mar 18
201598502	562 nm	44 nm	2017 Mar 18
228707509	562 nm	44 nm	2017 Apr 08
228707509	832 nm	40 nm	2017 Apr 08
228720681	832 nm	40 nm	2017 Mar 14
228720681	562 nm	44 nm	2017 Mar 14
228721452	562 nm	44 nm	2017 Mar 11
228721452	832 nm	40 nm	2017 Mar 11
228724899	562 nm	44 nm	2017 Mar 14
228724899	832 nm	40 nm	2017 Mar 14
228725791	562 nm	44 nm	2017 Mar 17
228725791	832 nm	40 nm	2017 Mar 17
228725972	832 nm	40 nm	2017 Mar 17
228725972	562 nm	44 nm	2017 Mar 17
228729473	832 nm	40 nm	2017 Apr 03
228729473	832 nm	40 nm	2017 May 19
228729473	562 nm	44 nm	2017 Apr 03
228729473	562 nm	44 nm	2017 May 19
228732031	832 nm	40 nm	2017 Apr 05
228732031	562 nm	44 nm	2017 Apr 05
228735255	832 nm	40 nm	2017 Mar 10
228735255	562 nm	44 nm	2017 Mar 10
228736155	562 nm	44 nm	2017 Apr 05
228736155	832 nm	40 nm	2017 Apr 05
228739306	562 nm	44 nm	2017 Mar 09
228739306	832 nm	40 nm	2017 Mar 09
228748383	832 nm	40 nm	2017 Mar 18
228748383	562 nm	44 nm	2017 May 19
228748383	832 nm	40 nm	2017 May 19
228748383	562 nm	44 nm	2017 Mar 18
228748826	562 nm	44 nm	2017 Mar 09
228748826	832 nm	40 nm	2017 Mar 09
228758778	562 nm	44 nm	2017 Apr 08
228758778	832 nm	40 nm	2017 Apr 08
228758948	832 nm	40 nm	2017 Mar 10
228758948	562 nm	44 nm	2017 Mar 10
228763938	562 nm	44 nm	2017 May 19
228763938	832 nm	40 nm	2017 May 19
228763938	562 nm	44 nm	2017 Mar 18
228763938	832 nm	40 nm	2017 Mar 18
228801451	832 nm	40 nm	2017 Mar 11
228801451	562 nm	44 nm	2017 Mar 11
228804845	562 nm	44 nm	2017 Mar 10
228804845	832 nm	40 nm	2017 Mar 10
228809391	562 nm	44 nm	2017 Mar 10
228809391	832 nm	40 nm	2017 Mar 10
228809550	832 nm	40 nm	2017 Mar 18
228809550	562 nm	44 nm	2017 Mar 18
228846243	832 nm	40 nm	2017 Mar 17
228846243	562 nm	44 nm	2017 Mar 17
228849382	832 nm	40 nm	2017 May 20
228849382	562 nm	44 nm	2017 May 20
228888935	832 nm	40 nm	2017 Mar 17
228888935	562 nm	44 nm	2017 Mar 17
228894622	832 nm	40 nm	2017 Mar 09
228894622	562 nm	44 nm	2017 Mar 09
228934525	562 nm	44 nm	2017 Mar 09
228934525	832 nm	40 nm	2017 Mar 09
228964773	562 nm	44 nm	2017 Mar 18
228964773	832 nm	40 nm	2017 Mar 18
228968232	832 nm	40 nm	2017 Mar 18
228968232	562 nm	44 nm	2017 Mar 18
228974324	832 nm	40 nm	2017 Mar 10
228974324	562 nm	44 nm	2017 Mar 10
228974907	562 nm	44 nm	2017 Mar 18
228974907	832 nm	40 nm	2017 Mar 18
229004835	562 nm	44 nm	2017 Mar 11
229004835	832 nm	40 nm	2017 Mar 11
229017395	832 nm	40 nm	2017 Mar 18
229017395	562 nm	44 nm	2017 Mar 18
229103251	832 nm	40 nm	2017 Mar 09
229103251	562 nm	44 nm	2017 Mar 09
229131722	832 nm	40 nm	2017 May 19
229131722	832 nm	40 nm	2017 Mar 10
229131722	562 nm	44 nm	2017 May 19
229131722	562 nm	44 nm	2017 Mar 10
229133720	562 nm	44 nm	2017 Mar 11
229133720	832 nm	40 nm	2017 Mar 11

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Table 10.  TNG/HARPS-N Results

EPIC	Tobs	RV	BIS	FWHM	log(RHK)	B − V	Texp	S/N
	(BJDTDB)	(km s−1)	(km s−1)	(km s−1)		(mag)	(s)	(5500 nm)
228801451	2457782.629699	22.960809 ± 0.001844	−0.012789	7.175241	−4.5707 ± 0.0098	0.873	1800.0	48.8
201595106	2457782.687224	0.692781 ± 0.002263	−0.022588	6.965865	−4.9714 ± 0.0273	0.703	2400.0	45.0
201437844	2457762.701586	−3.449696 ± 0.005740	0.037015	20.649605	−4.8647 ± 0.0058	0.451	1200.0	101.6
201437844	2457774.738143	−3.441043 ± 0.005931	0.045533	20.699375	−4.8584 ± 0.0060	0.451	1800.0	98.7
201437844	2457774.759707	−3.441611 ± 0.006562	0.073457	20.632207	−4.8629 ± 0.0071	0.451	1800.0	90.0

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Another possibly interesting RV target is K2-257 b, a sub-Earth-size planet orbiting a nearby M dwarf. Although the planet's radius is only ${0.83}_{-0.05}^{+0.06}$ ${R}_{\oplus }$, the Doppler semi-amplitude could be as high as ∼1 m s⁻¹ due to the low mass of the host star and the planet's short orbital period. The host star is moderately bright (Kp = 12.873, J = 10.477 mag), so this presents an opportunity to directly measure the mass of a sub-Earth with one of today's high-precision optical or NIR spectrographs. Such a measurement would yield the planet's density and constrain its composition, as well as improve our knowledge of the mass–radius relation for small planets. The only other sub-Earth-size planet known to transit a similarly bright M dwarf is Kepler-138 b, for which the mass has been measured only via TTVs (Jontof-Hutter et al. 2015; Almenara et al. 2018).