adsabs/AstroCLIMB huggingface dataset:
Paper: The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts
Authors: Ariane Deslières, Charles Cadieux, René Doyon, Étienne Artigau, Neil J. Cook, Clémence Fontanive, Thomas Vandal
Figure caption: The high-cadence part of the FWHM time series shows the  ∼30 days rotation period. The vertical blue dashed line represents the HARPS fiber upgrade. The green curve shows the mean prediction of the best-fit quasiperiodic Gaussian process with its 1σ confidence envelope.
Paper: The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts
Authors: Ariane Deslières, Charles Cadieux, René Doyon, Étienne Artigau, Neil J. Cook, Clémence Fontanive, Thomas Vandal
Figure caption: Posterior distributions of the activity model parameters. Contours denote the 1σ, 2σ, and 3σ confidence level. The blue lines indicate the median of the distributions, and the vertical black dashed lines represent the 16th and 84th percentiles.
Paper: The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts
Authors: Ariane Deslières, Charles Cadieux, René Doyon, Étienne Artigau, Neil J. Cook, Clémence Fontanive, Thomas Vandal
Figure caption: Posterior distributions of Model 1 parameters. Contours denote the 1σ, 2σ, and 3σ confidence level. The blue lines indicate the median of the distributions, and the vertical black dashed lines represent the 16th and 84th percentiles.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: The merged UVIT images obtained from five observations of IC 4329a in the NUV N245M (left panel) and FUV F154W (right panel) bands. The part of the field enclosed by the white colored dashed ellipse in each of the images is common to all five observations, and only this part of the field has been used for making the catalog. The common FOV in the NUV filter is centered at α = 207.31778° and δ = –30.30287° and measures 470 ﹩{{\rm{arcmin}}}^{2}﹩ in area, and the common FOV in the FUV filter is centered at α = 207.31706° and δ = –30.30465° and measures 423 ﹩{{\rm{arcmin}}}^{2}﹩ in area. The Seyfert galaxy IC 4329a and some other extended sources that are discussed in Sections 4.5 (sources 1–6 in the image) and 4.6 (sources 7 and 8 in the image) are marked with green-colored regions.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Detection of an extended source, a galaxy in this case, in the NUV band image using two different sets of detection criteria. The green and red ellipses in both the images indicate the extraction regions of the detected sources, while the source ID in the corresponding catalog file is mentioned next to each source region. Left panel: Initial detection of the galaxy by SExtractor as a group of several closely spaced sources due to its clumpy structure in the UV band when we used the detection parameters of the main configuration file as listed in Table 3. Right panel: Proper detection of the galaxy as a single extended source when the detection parameters listed in auxiliary catalog 5 column in Table 4 are used instead.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: The distributions of background counts per pixel for the NUV (left panel) and FUV band (right panel) images. The distributions were generated using ≈ 1000 square boxes of size 5 × 5 pixels placed across the image. The dotted curves show the best-fitting Gaussian profiles. We quote the mean background level (B) and its error (σB) in counts per pixel in the two panels for the NUV and FUV bands.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: The radial profile of HD 120190 used for PSF measurement in the NUV field. The orange curve shows the fitted curve of a Moffat function added with a constant for background value.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Limiting magnitudes in the FUV/F154W and NUV/N245M bands as a function of (a) exposure time for an SNR of 5 and (b) SNR for the actual FUV and NUV exposure times. The dashed lines in (a) represent the net FUV and NUV exposure times for the IC 4329A field. Our choice of an SNR of 5 for the source detection is marked as a dotted line in (b).
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Cumulative histogram of calculated SNR of all the sources in the NUV (left panel) and the FUV (right panel) field.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: The histogram of AB magnitude of all the sources in the NUV (left panel) and the FUV (right panel) field for sources above SNR of 5.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Four-way relay tracking link. At time ﹩{t}_{1}﹩, the ground station initiates the transmission of an uplink signal to the relay satellite. At time ﹩{t}_{2}﹩, the signal propagates through the relay satellite. At time ﹩{t}_{3}﹩, the lander receives and processes the signal via the forward link. At time ﹩{t}_{4}﹩, the signal is relayed through the relay satellite via the reverse link. At time ﹩{t}_{5}﹩, the signal returns to the ground station. ﹩{\rho }_{1}﹩ to ﹩{\rho }_{4}﹩ represent the range of observations of each link.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Formal uncertainty and relative true error of tidal Love number and lander positions for different orbital inclinations. The left panel represents the estimated results of the Love numbers, while the right panel represents the estimated results of the lander’s coordinates. The formal uncertainties are plotted as lines and the relative true errors are plotted as bars.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Formal uncertainty and the relative true error of tidal Love number and lander positions for different lander positions. The left panel represents the estimated results of the Love numbers, while the right panel represents the estimated results of the lander’s coordinates. The formal uncertainties are plotted as lines, and the relative true errors are plotted as bars.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Sensitivity of four-way range observations with respect to ﹩{k}_{2}﹩, ﹩{h}_{2}﹩, and ﹩{h}_{2}﹩ for different orbital inclinations of the relay satellite. The sensitivity of ﹩{k}_{2}﹩ is plotted as a blue “x,” that of ﹩{h}_{2}﹩ is plotted as an orange “+,” and that of ﹩{l}_{2}﹩ is plotted as green dots.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Sensitivity of four-way range observations with respect to ﹩{k}_{2}﹩, ﹩{h}_{2}﹩, and ﹩{l}_{2}﹩ for different lander positions, panels (a), (b), and (c) represent the sensitivity of the inclination of 76°, and panels (d), (e), and (f) represent the sensitivity for the inclination of 86°. The sensitivity of ﹩{k}_{2}﹩ is plotted as a blue “x,” that of ﹩{h}_{2}﹩ is plotted as an orange “+,” and that of ﹩{l}_{2}﹩ is plotted as green dots.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Horizontal (left) and vertical (right) tidal displacement for different lander positions, including both Sun- and Earth-induced tides. The displacement of the nearside is plotted in orange, that of the South Pole-Aitken basin is plotted in blue, and that of the farside is plotted in green.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Normalized correlation coefficients between the solved global parameters for different orbital inclinations of the relay satellite.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Lunar surface positions of three landers. Subplots (a), (b), and (c) correspond to Lander A, Lander B, and Lander C, respectively. Lander A (87°S,172°E, −3457.08 m) is located in the South Pole-Aitken basin, Lander B (6°N,27°E, −2567.0 m) is located in Mare Tranquillitatis, and Lander C (37°S,179°W, −6359.0 m) is located in the Leibnitz crater.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Normalized correlation coefficients between the solved global parameters for different lander positions.
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Left: inferred posterior surface for the tested grid of BT-SETTL (CIFIST 2011/2014) models fit to photometry of H II 1348B assuming a Gaussian prior Teff = 2500 ± 300 K for a spectral type of M8 ± 1. The color map represents relative inferred posterior probability density. A cutout of the grid spacing is shown with light gray “x” markers, and locations of fitted models interpolated between grid points are shown with open circles. The likelihood surface (equivalent to taking a uniform prior on Teff) is shown with dark gray dashed contours. Purple and salmon “⋆” markers show the locations of inferred local posterior maxima for tested models (shown fitted to the observed photometry of H II 1348B in Figure 6). Right: corner plot of inferred Teff and ﹩\mathrm{log}(g)﹩ for 6.6 × 106 samples with added Gaussian noise drawn from the interpolated posterior with emcee  (D. Foreman-Mackey et al. 2013). Diagonal subplots show 200 bin histograms with KDEs overplotted in solid black. Dashed and dotted lines mark MAP estimates and 68% HPD regions for each parameter. The off-diagonal subplot shows inferred density with a 2D KDE and scattered samples below the lowest contour.
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Measured apparent photometry of H II 1348B from Table 2 is plotted in black with interpolated BT-SETTL (CIFIST 2011/2015) model spectra from MAP estimation plotted in salmon and purple. Synthetic photometry as integrated from the model spectra are shown in their respective colors with horizontal error bars spanning the shaded filter widths (ΔλFWHM). Nonphysical, very low, and very high ﹩\mathrm{log}(g)﹩ at grid edges are yielded by MAP estimation of the two posterior modes. The multiwavelength photometry of H II 1348 is inferred to be generally consistent with a late M spectral type, with no constraint on ﹩\mathrm{log}(g)﹩. The interpolated model spectra are smoothed with a Gaussian filter to an average spectral resolution of R  = 250 for the displayed wavelengths. Reduced chi-square values (χν) are computed for 3 degrees of freedom: Teff, ﹩\mathrm{log}(g)﹩, and R.
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Corner plot of the distribution of 107 posterior orbit samples fitted with orbitize!/MCMC (see Section 3.2). Diagonal subplots show 200 bin histograms of 1D marginalized distributions with KDEs overplotted in solid black. Dashed and dotted lines mark MAP estimates and bounds of 68% HPD regions. Solid contours in off-diagonal subplots mark 1.5, 1, and 0.5σ levels containing ∼67.5%, ∼39.3%, and ∼11.8% posterior probability. Contours are estimated from 2D KDEs, with samples scattered outside of the 1.5σ level. The distributions of ω, Ω, and τ have been shifted by constant offsets for readability. The marginalized distributions of ω and Ω show only one of two such degenerate modes present in the absence of RV constraints. MAP estimates and 68% HPD regions corresponding to both degenerate modes are annotated (separated by 180°) above the diagonal for these parameters.
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Top left: one hundred randomly selected posterior orbits of H II 1348B from fitting to relative astrometry using orbitize! with an MCMC sampler (S. Blunt et al. 2020). The orbits are projected into relative R.A. and decl. (Δα,  Δδ), with color indicating the year along the orbits. The lower limit of the color bar corresponds to the first relative astrometric epoch from J. Bouvier et al. (1997) and the upper limit is the mean epoch for the plotted orbits to complete their first orbit. Top right: in blue are the projected separation and position angle (ρ,  PA) of H II 1348B as a function of time. Gray tracks show the ρ and PA of the same 100 posterior orbits plotted on the left. Bottom: histograms of selected orbital elements for all 107 posterior orbits from the converged MCMC chains. Solid colored lines show KDEs of the marginalized distributions. Dashed and dotted black lines show the locations of the MAP estimates and boundaries of 68% HPD regions, respectively.
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Contrast curve for the sensitivity of our ﹩L^{\prime} ﹩ observations to companions as a function of the projected separation. A nominal distance to the H II 1348 system of 143.3 pc (Gaia Collaboration 2020) is assumed for the conversion of angular projected separation to astronomical units. In black is the mean contrast ratio required for retrieval within 5% of SNR = 5, while the shaded region shows the sample standard deviation across injections at 18 PAs. The observed ﹩L^{\prime} ﹩ contrast ratio and projected separation of H II 1348B on 2019 September 18 are plotted in orange, with the error bars (smaller than the marker) overplotted in black. Colored bars indicate expected ﹩L^{\prime} ﹩-band contrast ratios for substellar objects of varying masses at the assumed age of the Pleiades (112 ± 5 Myr; S. E. Dahm 2015) generated from the evolutionary models of I. Baraffe et al. (2003).
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Detector-plane (pixels) plot of relative astrometry performed for the H II 1348 system (see Section 3.1). The dashed lines indicate LMIRCam pixel boundaries after aligning images to a common center. The fuchsia points are the measurements obtained from negative artificial companion injections into each of the four data sets, with their mean value shown with a black outline and error bars. The purple points are the measurements obtained for each data set using the IDL GCNTRD program, with their mean value shown with a black outline and error bars. Inferred error bars on the four individual measurements with either technique are not shown for readability. The mean astrometric measurements and their uncertainties were computed as the inverse-variance weighted mean, where the variance was inflated by a factor of 2 to account for the only semi-independence between data sets (see Section 3.1.1).
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Median  ±  MAD lowest-temperature MCMC walker positions at each saved step in the converged MCMC chains. By visual inspection, the constant median and MAD values for each fitted parameter across 30,000 steps, along with clear distinctions from the priors, indicate that the chains have converged to the posterior distribution. Only every third sample was saved to reduce the correlation between steps (i.e., “thinning”), giving 107 samples for 1000 walkers at the lowest temperature across 30,000/3 = 10,000 thinned steps. The degeneracy in ω and Ω for fitting only to relative astrometric measurements means that these two parameters could equally likely both be offset by 180° ﹩(\mathrm{mod}\,360^\circ )﹩; see Section 3.2.2.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: Left: SN 1 velocity map. Right: SN 1 broadening map. While the velocity values of the blended [O II] doublet follow the values reported for SN 2 and SN 3 closely, the broadening values differ. Instead, they are uniformly between 100 and 120 km s−1. This is likely due to the fact that the two lines are completely blended.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: Left: SN 3 velocity map. Right: SN 3 broadening map. Although these findings were initially reported in M. Gendron-Marsolais et al. (2018), we include the LUCI-based fits here for posterity. We note that globally the values are similar to those calculated previously.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: Left: SN 2 velocity map. Right: SN 2 broadening map. The values reported for the SN 2 data follow the SN 3 data closely.
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: Left Panel: exoplanets on the mass–radius plane, where blue dots are the planets from PlanetS catalog with mass less than 120 M⊕, radius less than 10 R⊕, and the left red dot is for the planet K2-266 d, the right red dot is for the planet K2-266 e, dashed lines are adopted from L. Parc et al. (2024); Right Panel: exoplanets on the radius-density plane, where blue dots are exactly the same planets as in left panel, the lower red dot is for the planet K2-266 d, the upper red dot is for the planet K2-266 e, dashed lines are based on the results in L. Parc et al. (2024).
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: The CHEOPS transit light curves of planet K2-266 d (top, orange) and K2-266 e (bottom, purple). For each planet, we show the corrected light curve and best-fit model (left) as well as the residuals (right). The data are plotted with respect to the linear ephemeris from J. E. Rodriguez et al. (2018).
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: TTV plots for the planet K2-266 d (top panel) and the planet K2-266 e (bottom panel). The points with error bars are observations, where blue ones are for K2, green ones are for TESS, and orange ones are for CHEOPS. The purple crosses and lines are the best-fit model (described in the later part of Section 3), in which the 1st cross for the planet K2-266 d is at the time 2457915.44712 BJDTDB and the 1st cross for the planet K2-266 e is at the time 2457919.05692 BJDTDB.
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: The TESS transit light curves of planet K2-266 d (top, orange) and K2-266 e (bottom, purple). For each planet, we show the corrected light curve and best-fit model (left) as well as the residuals (right). The data are plotted with respect to the linear ephemeris from J. E. Rodriguez et al. (2018).
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: The periods and eccentricities of the planet K2-266 d (left panel) and the planet K2-266 e (right panel) at the end of simulation t = 105 yr. The gray points are for the results of 100 simulations. The black points with error bars are for the means and standard deviations of these gray points, and the blue points with error bars are for the best-fit solutions and the corresponding uncertainties.
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: The evolution of periods, semimajor axes, and orbital eccentricities of the best-fit solution during the final 104 yr of the simulation. The top panels are for the planet K2-266 d and the bottom panels are for the planet K2-266 e.
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: The corner plot of 10-parameter MCMC fitting. For plotting convenience, we define Δpd ≡ pd − 14.69131 and Δpe ≡ pe − 19.49367 here.
Paper: Toward High-precision Mass Measurements of Two Sub-Neptunes in the K2-266 Planetary System Through Transit Timing
Authors: Ing-Guey Jiang, Li-Chin Yeh, Billy Edwards, Ming Yang, Keivan G. Stassun, Napaporn A-thano
Figure caption: The histogram of MEGNO indicators of 100 simulations.