adsabs/AstroCLIMB huggingface dataset:
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Sample TTV time series from a b:c = 3:2 pair at the end of Run D. This pair (subscript 1 for the inner member and 2 for the outer member) has a “well-defined” TTV phase: transiting conjunctions (marked by vertical dashed red lines) occur consistently before TTV zero-crossings with a time-averaged phase difference of 〈ΦTTV〉 ≃ −79∘. Blue points are simulation data and yellow solid curves are sine-wave fits, with the fitted Psuper labeled on the right.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: A library of diverse chains and their outcomes after 100 Myr of dynamical evolution. Initial (top) and final (bottom) neighboring planet period ratios for type (i) chains initially containing six planets (left column) and type (ii) chains initially containing four planets (right column).
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Sample TTV time series for a c:d = 2:1 pair for which a TTV phase is not well-defined. The sine-wave fits (yellow solid curves) are poor and yield discrepant values for Psuper. Also, no transiting conjunction is identified, even using the maximum value of Δttol.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: The observed transmission spectrum and retrieval analysis results. (a) Retrieval results showing the contributions of major atmosphere components. We excluded the contributions from CO and CH4 since they won’t be visible in the plot. (b) The transmission spectrum of planet HAT-P-14 b, extracted separately from fitting the light curves observed by NIRISS SOSS, NIRSpec NRS1 G395H, and NIRSpec NRS2 G395H. The fitted offset of 237 ppm between SOSS and NIRSpec is added to the SOSS part of the spectrum. The full model spectrum retrieved by PetitRADTRANS and the flat atmosphere model is also shown. (c) The residual spectrum obtained by subtracting the best-fit model from the observed transmission spectrum.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: The relationship between bin size and residual scatter for a particular spectroscopic bin of order 1 (left) and the white light curve of order 2 (right). We have chosen not to display the same plot for the SOSS order 1 white light curve, as the use of common-mode correction results in an underestimation of the residual scatters. The dashed blue line is the theoretical decrease for white noise (proportional to ﹩1/\sqrt{N}﹩) and the horizontal red dashed line is an estimate of the red noise.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: Spectrophotometry extraction step of FIREFLy. We choose aperture widths for each spectral order so that the out-of-transit scatter for the transit light curve is minimized. We extract the spectrophotometry bounded by the boxed regions.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: White light curve fits for both order 1 and order 2. Top: the white light curves for SOSS order 1 and order 2, respectively shown on the left and right. The reduced χ2 for SOSS order 1 is 1.01 and that for SOSS order 2 is 1.02. Bottom: the residuals for the white light curve fits.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: 1/f noise and background removal steps of FIREFLy. (a) The background model for SOSS measured during commissioning; a jump of flux levels due to the zodiacal light can be seen at x ∼ 700. (b) The same frame as Figure 1 after background subtraction. (c) The 1/f noise shown in the frame. (d) The same frame as (b) after 1/f destripping.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: Products of FIREFLy reduction for the NIRISS-SOSS HAT-P-14 b data set at different steps up until cosmic rays removal. (a) Raw uncalibrated frame in data numbers (DN). (b) After stage 1 calibration. (c) After bad and hot pixels correction. (d) After cosmic-ray removal.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: Plots of the relationship between bin size and residual scatter for detectors NRS1 and NRS2 of NIRSpec. The dashed blue line is the theoretical decrease for white noise (proportional to ﹩1/\sqrt{N}﹩) and the horizontal red dashed line is an estimate of the red noise.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: White light curve fits for detectors NRS1 and NRS2 of NIRSpec, along with the residuals between model and observed light curves.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: The residual Root Mean Squarerms of transit depth calculated with different numbers of pixels per wavelength bin, from binning before (prebinning) or after (postbinning) the light curve fit. The dashed black line is the theoretical decrease for rms (proportional to ﹩1/\sqrt{N}﹩).
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: Left: dilution-corrected SOSS transmission spectrum overplotted on the original transmission spectrum. Right: the maximum possible dilution factor introduced to the transmission spectrum from the nearby M-dwarf companion from 0.6 to 2.8 μm. The spectrum is generally unaffected by the possible dilution; in particular, the water bands are still present in the spectrum after the correction.
Paper: Unveiling the Atmosphere of the Super-Jupiter HAT-P-14 b with JWST NIRISS and NIRSpec
Authors: Rongrong Liu, Le-Chris Wang, Zafar Rustamkulov, David K. Sing
Figure caption: The posterior distribution of model atmosphere parameters for HAT-P-14 b, assuming isothermal temperature and free chemistry. (both Pcloud and the mass fractions of atmosphere components are in ﹩{\mathrm{log}}_{10}﹩scale).
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Periodogram of out-of-transit data from TESS (blue line). The Lomb–Scargle periodogram is designed to identify periodic signals within unevenly spaced data. Vertical red lines are drawn to indicate the period of the planet, 4.81 days, and the suspected stellar rotation period of 5.40 ± 0.09 days. The horizontal lines represent 10%, 1%, and 0.1% false-alarm levels calculated from 100 random draws. The inset shows the uncertainty on the stellar rotation peak and demonstrates that the data can conclusively resolve the stellar rotation and planetary signals. There is a signal at the planet’s period even though its primary transits have been removed before calculating this periodogram.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Top: zero-pointed and phased RVs including both the HIRES (blue squares) and NEID (red triangles and circles) data. The two HIRES data points that fall in the shaded region are affected by the RM effect and thus excluded. The two data sets exhibit similar variational amplitude consistent with the upper bound from Z17. Bottom: phase-folded light curve from TESS with bins of 100 points, demonstrating the existence of HAT-P-67 b.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Correlations between the RVs and stellar activity indicators dLW, CRX, CaIRT, Hα, NaD, PaD, and NaNIR (defined in M. Zechmeister et al. 2018). NEID1 data are plotted in blue, and NEID2 data are plotted in orange. The data from NEID1 and NEID2 are normalized to their respective zero-points. We calculate the uncertainties of the Spearman correlation coefficients using bootstrap resampling. The differential line width, Paschen delta, and sodium near-infrared indicators have statistically significant (p < 0.05) monotonic correlations with the RVs, with ρ = 0.293 ± 0.101, −0.239 ± 0.129, and 0.581 ± 0.076 as obtained from a Spearman rank correlation test. A visual trend is not always immediately apparent, due to the rank correlation test ignoring the actual values of the data.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: RV data points with overplotted model containing one Keplerian. The gray bands represent 68%, 95%, and 99% confidence intervals. The data uncertainties are drawn as thick error bars, and the thin error bars represent the jitter added in quadrature to the data uncertainties. This model does not include a GP, resulting in large jitter values.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Phased RVs and best-fit model, without a GP (left) and with a quasi-periodic GP (right). The data points on the right are detrended by the GP component of the model, which effectively improves agreement between the data and the model.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: l1 periodogram for HAT-P-67 RVs. Labeled in orange are the periods of the peaks with Bayes factors ≥2.0. The Bayes factors of the signals, in order of increasing period, are 6.7, 10.3, and 2.0, respectively. The p-values of the peaks are 2.85 × 10−1, 2.55 × 10−2, and 1.48 × 10−4, respectively.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Light curve for HAT-P-67 from TESS, phased to the planetary orbital period. Each point here is the result of binning 400 2-minute-cadence points in the TESS photometry. The light curve was first phase-folded and then binned.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Out-of-transit data from TESS phased to the strongest peak of 5.40 days. Blue points represent raw data binned by 10, and white circles represent bins of 1000. The best-fit sinusoidal model phased to the Lomb–Scargle peak is overplotted in black.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Same as Figure 8, but for the full model, which includes a by-instrument quasi-periodic GP component. The blue and red lines represent the GP component for the HIRES and NEID data, respectively.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: O–C plot of midtransit times. No significant short- or long-term deviations are found.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Phased raw (blue) and binned (white circles) photometry data points. Best-fit models (black lines) and residuals are also included.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Model for the self-consistent tidal evolution of the HAT-P-67 system. We plot as black lines the semimajor axis (left), scaled semimajor axis a/R* (middle), and orbital decay rate dP/dt (right) as functions of time in Gyr. As the tidal quality factor ﹩{Q}_{* }^{\prime} ﹩ for the host star is unknown, we model four potential cases spanning the plausible range of hot Jupiter host stars (A. J. Barker 2020; N. N. Weinberg et al. 2024): 105 (dotted lines), 105.5 (dashed–dotted lines), 106 (dashed lines), and 107 (solid lines). We start the planet at a semimajor axis of 0.06303 au (corresponding to its present-day period of 4.8 days), assuming Qp = 106, a circular orbit, synchronized rotation and revolution, and a small nonzero obliquity of 2.∘2 (D. Sicilia et al. 2024). We evolve the planet from its current age of 1.46 Gyr to the point at which it reaches its host star’s radius. If HAT-P-67’s ﹩{Q}_{* }^{\prime} ﹩ is on the higher end of the typical range, the planet will be engulfed in about 500 Myr; on the other hand, if HAT-P-67’s ﹩{Q}_{* }^{\prime} ﹩ is on the lower end of the typical range similar to that of WASP-12 (S. W. Yee et al. 2020), then the planet will be tidally disrupted in 150–250 Myr, demonstrating HAT-P-67 b to be a doomed world. Regardless of which scenario occurs, this orbital decay is unlikely to be detectable for any plausible ﹩{Q}_{* }^{\prime} ﹩ value.
Paper: The Milky Way Project MOBStIRS: Parameterizing Infrared Stellar-wind Bow Shock Morphologies with Citizen Science
Authors: Angelica S. Whisnant, Matthew S. Povich, Nikhil Patten, Henry A. Kobulnicky
Figure caption: Image of an IR bow shock created using 24 μm data from MIPSGAL (red) and 8.0 μm and 4.5 μm data from GLIMPSE (green and blue, respectively). Overlaid are the IR bow shock shape parameters of interest: R0 (measured from the driving star to the apex of the arc), R90 (the distance from the driving star to the arc, perpendicular to the symmetry axis of the bow shock), and Rc (the best fitting circle along the arc of the bow shock).
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Full light curves from TESS. Data from Years 2, 4, and 6 of the TESS mission are shown in the top, middle, and bottom rows, respectively. The data visually suggest a stellar rotation period of a few days. Stellar activity is strongest in Year 2, weakens for Year 4, and returns to elevated levels in Year 6, demonstrating starspots+rotation as a probable cause of the variations.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Corner plot for HAT-P-67 A fit.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Top: mass–radius plot of known transiting exoplanets with equilibrium temperatures greater than 1000 K. The original location of HAT-P-67 b from Z17 is marked by a blue circle, and the updated location from this work is indicated by a red star. HAT-P-67 b is the largest known hot giant planet and is one of only four planets to cross the ρ = 0.1 g cm−3 boundary. Bottom: zoomed-in version, with curves representing ρ = 0.07 and 0.1 g cm−3. The only other planet with ρ < 0.07 g cm−3 is WASP-193b.
Paper: The Milky Way Project MOBStIRS: Parameterizing Infrared Stellar-wind Bow Shock Morphologies with Citizen Science
Authors: Angelica S. Whisnant, Matthew S. Povich, Nikhil Patten, Henry A. Kobulnicky
Figure caption: Screenshot of the interface used by the citizen scientists to make classification drawings on each image.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Evolution of a 1.73 M⊙ star from MESA in luminosity–Teff space. The current parameters of HAT-P-67 A are plotted as the black plus sign, and the gray numbers represent the logarithm of the age of the star in years.
Paper: A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 b
Authors: Gavin Wang, William O. Balmer, Laurent Pueyo, Daniel Thorngren, Stephen P. Schmidt, Le-Chris Wang, Kevin C. Schlaufman, Guðmundur Stefánsson, Zafar Rustamkulov, David K. Sing
Figure caption: Corner plot for joint (photometry+RVs) fit that includes one planet and a quasi-periodic GP. We adopt this fit as final. We include only the planetary parameters and GP parameters for the NEID data for clarity.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Observing geometry as a function of Day of Year (DOY, 1 = UT 2022 January 1). Heliocentric (rH) and geocentric distances (Δ), shown as solid black and long-dashed blue lines, respectively, are referred to the left-hand vertical axis. The phase angle (α) and orbital plane angle (δi), shown as short-dashed red and dashed–dotted orange lines, respectively, refer to the right-hand axis.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Composite of BAA (small green circles) and NOT (large red circles) photometry as a function of time expressed as Day of Year (DOY). All measurements refer to a 9″ photometry aperture except those shown with upward-pointing error bars, which denote limits to the brightness forced by the use of smaller photometry apertures. The dashed black line shows the expected variation of a bare nucleus having an absolute magnitude H = 13.4. Model 1 (solid red line) shows a fit with heliocentric and spatial indices m = 4.0, n = 2, respectively, while Model 2 (dashed blue line) has m = 4.5, n = 1 (see Equation (A2)). Both models assume a phase function of 0.02 mag degree–1.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Close-up of Outburst D (see Figure 6) with a black line added to guide the eye. The zoom box shows the ultra-rapid rise portion of the lightcurve with a tick mark separation on the x-axis of 0.005 days, or about 7 minutes.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Composite showing morphological development of 12P in a subset of the NOT R-band images, with the dates and heliocentric distances of each indicated. The comet is centered in each panel. Note that different panels have different scales, as marked.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: R-filter images of 12P Outburst A, each of 90 s integration from the NOT. Each panel has north to the top and east to the left. A 60″ scale bar, corresponding to about 150,000 km at the comet, applies to all panels and is shown in the upper left. The projected antisolar direction and the negative of the heliocentric velocity vector are shown as solid and dotted arrows, respectively.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Sunward extent of the coma in the 2023 July–August period as a function of date. Lines in the figure show simple radiation pressure models for particles having radiation pressure efficiencies β = 10−3, 10−2, 10−1, and 1, as marked.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Fading portion of the Outburst D lightcurve with background subtracted, converted to flux normalized at the peak as a function of time measured from the peak t0 = 685.1. The dashed line shows a weighted least-squares power-law fit of slope −2.5, giving a differential size index γ = 4.2 ± 0.2.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Outburst photometry from BAA as a function of time expressed as Day of Year (DOY). The major outbursts are labeled A–G. A fit of Equation (B1) to the nonoutburst photometry with m = 4.0, n = 2 is shown as a solid red line.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: The excess brightness of each outburst is plotted as a function of the heliocentric distance at the outburst time, with ±0.2 mag (1σ) uncertainties on the excess. Letters mark the individual outbursts.
Paper: Multiple Outbursts of Halley-type Comet 12P/Pons–Brooks
Authors: David Jewitt, Jane Luu
Figure caption: Mass-loss rate between outbursts as a function of heliocentric distance. The solid black line shows a least-squares power-law fit to the data.
Paper: Observations and Studies on the Transiting Systems HAT-P-36, XO-2 and WASP-76
Authors: Weilong Wang, Shenghong Gu, Xiaobin Wang, Leilei Sun, Byeong-Cheol Lee, Chi-Tai Kwok, Ho-Keung Hui, Jiangpei Dou, Yue Xiang, Dongtao Cao, Fukun Xu
Figure caption: The MEGNO maps of the systems HAT-P-36 (top row), XO-2 (middle row) and WASP-76 (bottom row). Each row depicts three orbit configurations for the perturber: (i) coplanar and circular orbit; (ii) coplanar and slightly eccentric (e = 0.2) orbit; and (iii) inclined and slightly eccentric (e = 0.2) orbit, from left to right. The black dots represent the upper mass limits determined from the rms of the observed TTVs. The yellow curves are the constraints derived from the rms of the RV residuals. red regions indicate regular orbital configurations, while red regions indicate chaotic status.