adsabs/AstroCLIMB huggingface dataset:
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Radius as a function of the mass at multiple epochs from multiple evolution model grids: the COND model grid (solid lines) and the DUSTY model grid from Allard et al. (2001; dashed lines). The gray box represents the photometry-derived mass and radius from previous studies (Currie et al. 2014a; Daemgen et al. 2017). The gray point on the left is calculated using the radius and log(g) values from our joint retrieval. The dark gray point on the right is calculated using the radius and log(g) values from our low-resolution-only retrieval.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Corner plot comparing the posterior probability distributions of key parameters from our fixed and free P–T profile retrievals on our low-resolution spectrum using a gray cloud model and (a) an unrestricted spline pressure–temperature (P–T) profile, (b) a P–T profile fixed to a Sonora P–T profile (Marley et al. 2021a, 2021b), and (c) a P–T profile fixed to a Sonora model P–T profile and the reddening coefficient fixed to the best-fit stellar value from Bowler et al. (2014).
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Retrieved cloud opacity for our EddySed cloud model (orange), compared with the retrieved cloud opacity for our gray slab cloud model (green) as a function of the pressure, for our low-resolution-only fits (dashed lines) and our joint high-resolution and low-resolution fits (solid lines). The gray-shaded region represents the region of the atmosphere where the total contribution to flux is greater than 0.01%. For both cloud models we see that the in the low-resolution-only case, the clouds are placed deep in the atmosphere where they have minimal impact on the flux, and the inclusion of the high-resolution data requires the presence of clouds to explain the observed data.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Corner plot comparing the posterior probability distributions of key parameters from retrievals on our high-resolution spectrum for three different cloud models: a clear sky, a simple gray cloud deck, and EddySed condensate clouds composed of Fe and MgSiO3. We find identical posterior probability distributions regardless of the cloud model used.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Corner plot comparing the posterior probability distributions of key parameters from retrievals on our low-resolution spectrum for our three considered cloud models, a clear sky, a simple gray cloud deck, and EddySed condensate clouds composed of Fe and MgSiO3.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Contribution functions for the best-fit models for our low-resolution (left) and high-resolution (right) retrievals.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Corner plot comparing the posterior probability distributions of key parameters from joint retrievals on our low-resolution and high-resolution data sets for our three considered cloud models, a clear sky, a simple gray cloud deck, and EddySed condensate clouds composed of Fe and MgSiO3.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Best-fit model to the SNIFS optical spectrum of the unresolved binary ROXs 42B (top panel) and error-weighted residuals (lower panel). The best-fit model is shown in green, with randomly drawn samples shown in gray.
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: Posterior distribution for the simultaneous FUV and X-ray spectrum in the oxygen region. The distribution compares each pair of free parameters of the fit with two-dimensional histograms. The parameters in the plot correspond to the following quantities: N H is the neutral hydrogen column density in units of 1021 cm−2 along the line of sight; z  v  is the velocity shift in km s−1; ﹩\mathrm{log}({\mathrm{norm}}_{\mathrm{bb}})﹩ is the logarithm of the blackbody normalization; N dust is the total column density of dust in 1018 cm−2; b refers to the line velocity broadening in km s−1; O II, O III, and O IV correspond to the logarithmic ionic column densities in cm−2; and Oabund is the O abundance scale factor relative to Lodders & Palme (2009).
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: COS/FUV absorption lines and best-fit model for Fe II, S II, C I, and C II in velocity space.
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: Comparison of the different abundance tables for every element, where ref 1: Anders & Grevesse (1989); ref 2: Grevesse & Sauval (1998); ref 3: Wilms et al. (2000); ref 4: Lodders (2003); ref 5: Lodders & Palme (2009); ref 6: Asplund et al. (2009); ref 7: Asplund et al. (2021); and ref 8: Nieva & Przybilla (2012).
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: The posterior distribution for S II is plotted with two-dimensional histograms comparing each pair of free parameters. The contours represent the confidence levels of 1σ, 2σ, etc. N S II  is the logarithmic ionic column density in cm−2, z  v  is the velocity shift of each component in km s−1, and b is the velocity broadening in km s−1. The inset displays the identical posterior distribution, where the velocity-broadening parameter is fixed to the fitted value.
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: Best fit in the O K-edge and O I line profile in the HST/COS. Top: XMM-Newton/RGS. Bottom: HST/COS.
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: Best fit in the Fe L-edges toward Cygnus X-2. Top: Chandra/HETGS spectrum. Bottom: XMM-Newton/RGS spectrum.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Example of the plane-parallel ray model of illumination of an exoplanet in which the yellow arrows represent the rays of light incident on the exoplanet at right. For such exoplanets, the instellation is proportional to the cosine of the zenith angle (﹩{\gamma }^{{\prime} }﹩) because all angles of incidence (ξ) are equal to the zenith angle. The illumination extends to cover only the hemisphere of the exoplanet facing its host star.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Illustration of a point P on the planet being illuminated by a point Q on the host star with associated directions and lengths. The point Q is located at distance r  q  from O  p  and ﹩{\rho }^{{\prime} }﹩ from P. The star’s center is located at O  s  a distance r  s  from the center of the planet O  p . Note that ﹩\cos {\vartheta }_{i}﹩ is now given by ﹩{\hat{r}}_{Q}\cdot \hat{p}﹩, and ﹩\cos \xi ﹩ by ﹩\hat{p}\cdot \hat{{\rho }^{{\prime} }}﹩, similar to Figure 3, but with the shift of  r   s  to  r   Q  =  r   s  + d  r   Q  and  ρ  to ﹩{{\boldsymbol{\rho }}}^{{\prime} }={\boldsymbol{\rho }}+d{{\boldsymbol{r}}}_{Q}﹩. Adapted from Carter (2018).
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Intensity maps for KELT-9 b using six methods to calculate the illumination. In the figure, I pt,starry and I ext,starry use starry’s point-source and extended-source models, and ﹩{I}_{\mathrm{ext},\cos \xi }﹩ uses Equation (28) as described in Section 2.4.2. ﹩{I}_{\mathrm{ext},\cos \xi \cos {\theta }^{{\prime} }}﹩ uses the methods described in Section 2.2 by Equations (9), (10), and (11), and I full is the analytical solution to Equation (11) within the fully illuminated zone given by Equation (26). For the numerical models (I ext,starry, ﹩{I}_{\mathrm{ext},\cos \xi \cos {\theta }^{{\prime} }}﹩, and ﹩{I}_{\mathrm{ext},\cos \xi }﹩), 25 source points were used. Note that I ext,starry and ﹩{I}_{\mathrm{ext},\cos \xi }﹩ suggest greater illumination compared to the other methods, with I ext,starry overestimating the intensity at the substellar point by 118.8263 ppm of I star compared to I full. See text for descriptions of each method listed in the maps. The black dashed line delimits the fully illuminated zone. The white dotted lines are contours lines, where 100% is the maximum intensity across all six maps.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Shown are the illumination zones of an exoplanet (right) due to illumination by a spherical star (left) of radius R  s  illuminating a spherical exoplanet of radius R  p , whose centers are separated by distance r  s . The angles shown delimit the fully illuminated zone (η full, in yellow), the penumbral zones (η pen), and the unilluminated zone (η un, in black). The penumbral zone nearer the host star (orange) is denoted PZ1 in the text, and that farther from the host star (maroon) is denoted PZ2. The inner tangents are associated with the dashed lines, the outer tangents with the dotted–dashed lines, and the penumbral zones with the dotted lines. Figure adapted from Carter (2022).
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Shown is the geometry required to determine the geometric depth of the eclipse (λ), which defines the polar angle on the host star at which the horizon at P intersects the apparent stellar disk. A: the horizon intersects the host star such that more than half of the apparent disk is visible. This situation applies for points within PZ1 for which ﹩\alpha \leqslant \displaystyle \frac{\pi }{2}﹩, δ = π − ∣λ∣ − ∣β∣, and ﹩| \beta | =\displaystyle \frac{\pi }{2}-\alpha ﹩. B: the case for P for which the horizon blocks more than half of the apparent stellar disk, i.e., for points within PZ2. In this case ﹩\alpha \gt \displaystyle \frac{\pi }{2}﹩, δ = π − ∣λ∣ − ∣β∣, and ﹩| \beta | =\alpha -\displaystyle \frac{\pi }{2}﹩. Adapted from Carter (2018).
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Intensity maps for Trappist-1 d using six models of illumination. See text and Figure 6 for labeling conventions. Note that the differences between the models are less pronounced than seen in Figures 6 and 7 due to the much smaller value of R  p /r  s .
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Illustration of a point P on an exoplanet with origin O  p  located at ﹩{\boldsymbol{p}}=x\hat{x}+y\hat{y}+z\hat{z}﹩ being illuminated by a point-source host star at ﹩{{\boldsymbol{r}}}_{s}={x}_{s}\hat{x}+{y}_{s}\hat{y}+{z}_{s}\hat{z}﹩ with associated directions, vectors, and coordinates.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Differences in the intensities generated by each method along the intensity equator of KELT-9 b. Note that they are always greatest at the substellar point. The black- and cyan-dotted vertical lines delimit the unilluminated and fully illuminated zones, respectively, where the penumbral zone is located between the two lines. See legend for subtractions. The inset is a zoomed-in plot within the illuminated region to highlight the smaller differences.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Intensity maps for Kepler-91 b using six models of illumination. See text and Figure 6 for labeling conventions. As in Figure 6, I ext,starry overestimates the illumination compared to I full.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Intensity at the substellar point for KELT-9 b analogs using six models of illumination. In all cases, the models converge for large star–planet separations. The green dashed line marks the scaled star–planet separation given by a/R  s  using the parameters given in Table 2. See text for legend labeling conventions.
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Lower limits to the nucleus diameter of C/2019 E3 as functions of heliocentric distance assuming the observed activity is driven by sublimation of CO (a) and CO2 (b). Results in subsolar and isothermal scenarios are plotted as solid and dashed–dotted curves, respectively, in different colors representing different effective sizes of dust grains used for the computation. We conservatively assumed ﹩{ \mathcal X }=5﹩ for the ratio of the dust-to-gas mass production rates in the calculation. In addition, we adopted an empirical model by Womack et al. (2017) that is consistent with the CO measurements of comet C/1995 O1 (Hale–Bopp) and Centaur 29P/Schwassmann–Wachmann in the left panel, extrapolating it to greater heliocentric distances.
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Monte Carlo dust models of comet C/2019 E3 at six of the selected epochs. All of the images are scaled logarithmically. In each panel, the red and yellow arrows mark the position angles of the antisolar direction and the negative heliocentric velocity projected in the plane of the sky, respectively, and two scale bars of 10″ in apparent length (labeled) and 105 km projected at the observer-centric distance of the comet are shown in white and magenta, respectively. J2000 equatorial north is up and east is left.
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Comparison between periapsis distance (q), eccentricity (e), inclination (i), argument of periapsis (ω), longitude of ascending node (Ω), and reciprocal of the semimajor axis (a −1) of original Solar System barycentric J2000 ecliptic orbits of the four known ultradistant comets C/2010 U3, C/2014 UN271, C/2017 K2, and C/2019 E3 (color coded by bold symbols; see the legend in the upper left). Background dots in gray are other long-period comets, whose original orbits together with those of the three previously known ultradistant comets are based on the preferred solutions in the CODE catalog. Associated 1σ formal errors in the orbital elements of the ultradistant comets are also included in the plots. However, as they are in general much smaller than the displayed ranges here, they are basically invisible, except for C/2017 K2 in terms of its reciprocal of the semimajor axis.
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Effective scattering cross section of dust as a function of heliocentric distance, calculated from r-band data points measured with an aperture of 3 × 104 km in radius. Data points in different symbols correspond to measurements from different facilities. The dotted curve is the best-fit power law with heliocentric distance for the effective scattering cross section of dust. The overall trend is that the effective scattering cross section of dust increased monotonically as the comet approached the Sun.
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Total and net mass-loss rates of comet C/2019 E3 vs. heliocentric distance (dashed–dotted and solid curves, respectively) assuming different effective radii of dust grains (plotted in different colors). The best-fit effective scattering cross section of dust in the power-law form vs. heliocentric distance (see Section 3.2) was used.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Individual planet radii against their orbital periods and colored by their mass partitioning (Gilbert & Fabrycky 2020) for 649 planets (229 planetary systems). For planets colored gray (459 planets in 121 systems), we do not provide an estimate for the mass partitioning because the system has a planet missing from the steps outlined in Appendix A. In addition to our measurements for Kepler-323 and Kepler-104 (squares), LTT 1445 A, TOI-125, Kepler-30 and the Inner solar system are highlighted for comparison.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Planet densities vs. physical radii for Kepler-104 (dark blue), Kepler-323 (dark purple), solar system objects (red squares), and planets selected from the NASA Exoplanet Archive according to Appendix A (translucent). The Solar System objects include Mercury, Venus, Earth, Mars, Uranus, Neptune, Pluto, and the Moon. Non-solar-system objects are colored by their orbital period (see legend). The composition curves consistent with 100% Fe, 100% MgSiO3, and 67.5% MgSiO3 + 32.5% Fe are taken from Zeng et al. (2019), while the maximal collisionally stripped composition curve is taken from Marcus et al. (2010).
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Top: RVs for Kepler-323, from HIRES (yellow) over 80 nights between 2019 May and 2021 October combined with 48 RVs from HARPS-N (dark red; Bonomo et al. 2023). The blue line represents the best-fit Keplerian orbits. The residuals are shown in panel (b). Bottom: phase folded RVs and the corresponding best-fit Keplerian orbit for each individual planet. The red circles are the RVs binned in orbital phase.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: The posterior distribution of mass partitioning values, based on 1000 draws from the posteriors of the planet masses, for the systems described in Section 4.1. The solid black line represents the median mass partitioning of the sample. The dashed lines represent the best fit mass partitioning value for Kepler-104 (blue), Kepler-323 (purple), and the inner solar system (red). The shaded regions represent the 1σ errors.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Same as Figure 3, but with the y-axis corresponding to mass instead of density.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Same as Figure 1, but for Kepler-104
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Posterior distributions for all derived parameters from the Keplerian best-fit orbit of Kepler-323. There is no strong covariance between the masses of planets b and c