adsabs/AstroCLIMB huggingface dataset:
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Full FOV of the TWA 7 observation in the F444W filter. Each candidate is circled and labeled with C1–6. The lower right plot shows a zoom-in view of C4 in the F200W filter, while the upper right plot shows a zoom-in view of the inner region of the F444W observation after subtraction of the disk model to better show candidates C5 and C6.
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: Measurable contamination by a hypothetical plasma torus in the GJ 367 system. Top: model spectrum (S. Peacock, private communication) of the M dwarf star GJ 367 A (solid black), using stellar parameters Teff = 3560 K, ﹩\mathrm{log}g=4.78﹩ in cgs units, M = 0.44 M⊙, and [Fe/H] = 0, which are comparable to those from E. Goffo et al. (2023). Our spectrum was derived from a PHOENIX grid (F. Allard et al. 2012) model with updated treatment of M dwarf chromospheric non-LTE emission (S. Peacock et al. 2019a, 2019b), with flux scaled to replicate GALEX FUV photometry of GJ 367 A. Colored lines denote spectral contamination by a circumstellar torus of plasma supplied by volcanism from GJ 367 b. The atomic species carbon (blue), oxygen (red), sulfur (yellow), sodium (green), and potassium (purple) are present in ionization states I (solid), II (dashed), and III (dotted) at the levels implied by the value of τ provided in Table 1 and the outgassing rates provided in Table 2. While some intrinsic stellar absorption features are expected at GJ 367 A’s metallicity of Z = −0.01 ± 0.12, a plasma torus would enhance the strength of select features based on its composition. Bottom: absorption produced by a hypothetical GJ 367 b plasma torus relative to the expected flux as measured by HST COS, STIS, and WFC3 grisms and gratings. For wavelengths shorter than 300 nm, we bin every 0.1 Å to emulate HST COS and STIS echelle observations. At wavelengths longer than 300 nm, we bin every 2 nm to emulate HST STIS grating and WFC3 grism observations.
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: Stellar Alfvén radii of stars with measured masses, radii, and spin periods that are also known to host terrestrial exoplanets. For the 33 exoplanets that orbit at a < RA, magnetic confinement is strong enough to permit construction of plasma tori. Io is plotted in terms of Jupiter radii RJ; the Jovian Alfvén radius is sourced from R. L. J. McNutt et al. (1979) and T. W. Hill (1980). Targets in the gray region orbit outside of the stellar Alfvén radius. Conditions for being classified as a high-priority target, including the classification of GJ 367 b as highest priority, are described in Section 4.
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: Magnetospheric convection timescale τ over which mass injected into a plasma torus by an exoplanet at distance a/RA would be removed. Less time is required to remove mass when the injection occurs closer to the Alfvén radius. We calculate τ with Equation (10) using the same assumptions and exoplanets as in Figure 1, restricting the plot to show only exoplanets that orbit at a < RA. The value of τ for Io is sourced from F. Bagenal & V. Dols (2020).
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: Schematic illustration of the plasma torus (gray) built by a volcanically active exoplanet (red shaded circle) in orbit around a star (yellow circle), with a neutral cloud extending a few planetary radii ahead and behind the source exoplanet (dotted gray). (a) The torus major radius R = a + (3H/2) is the distance from the star’s center to the center of the tube. The minor radius r = 3H/2 is half the diameter of the tube. (b) The torus inner radius, rinner,​ is equal to the planet orbit distance, a. The outer radius router = a + 3H marks the edge of the warm torus and contains 90% of the torus mass. (c) The Alfvén radius RA typically lies much further out than router. The stellar magnetic field loops (in blue) switch from a closed to a radially outward and open geometry (A. ud-Doula & S. P. Owocki 2002) at the Alfvén radius.
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: The magnetospheric convection timescale shows a positive correlation with the tidal heating rate. This suggests that exoplanets that are well positioned for plasma torus construction will generally also receive the necessary tidal power to drive volcanism. This plot includes the 13 terrestrial exoplanets plotted in Figures 1 and 3 that had nonzero orbit eccentricities and orbited within their host stars’ Alfvén radii, marked on all figures as “high-priority targets.” GJ 367 b is considered the highest-priority target due to its high tidal heating power and long magnetospheric convection timescale. The values of τ presented here are the same as in Figure 3. Color indicates the V magnitude of the system, which is indicative of favorability for UV-optical spectroscopy.
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: Radiation magnetic confinement parameter ζ for the 33 exoplanets that orbit at a < RA identified in Figure 1. For all but eight of these targets, the magnetic pressure is at least 2 orders of magnitude greater than the radiation pressure, such that radiation pressure is unlikely to be capable of dispersing magnetically confined plasma. Targets in the gray region have ζ ≤ 100 such that their tori may be dispersed by radiation pressure.
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: The 13 high-priority exoplanets highlighted in this study as they appear on the XUV-driven cosmic shoreline. With increasing vertical distance above the shoreline, the likelihood of substantial volatile depletion rises.
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: The 13 high-priority exoplanets highlighted in this study as they appear on the thermal cosmic shoreline. With increasing vertical distance above the shoreline, the likelihood of substantial volatile depletion rises.
Paper: Discovery of a Variable Yellow Supergiant Progenitor for the Type IIb SN 2024abfo
Authors: Zexi Niu, 泽茜 牛, Ning-Chen Sun, Justyn R. Maund, Zhen Guo, Wenxiong Li, Meng Sun, 萌 孙, Jifeng Liu
Figure caption: Pre- and postexplosion images of the site of SN 2024abfo. Each panel is labeled with the instrument, band, and epoch. Details of the pre-explosion imaging are summarized in Table 1. All panels are aligned with north up and east to the left. Panel (a) and (b) have the same scale, with reference stars used for astrometric transformation between WFPC2 and SOAR circled in blue and SN site marked in red. The transformed SN position and its uncertainty are shown with the red circle in Panel (c). Two nearby sources detected in F814W image are indicated in cyan and green. Panels (c) to (i) show a same zoomed-in scale. About 20 common stars on SOAR and DECaLS/VISTA images are used for astrometric transformation. The transformed SN position as well as two nearby sources are also indicated in the same colors as in panel (a). The typical astrometric uncertainties for both DECaLS and VISTA are 0.4 pixels.
Paper: Discovery of a Variable Yellow Supergiant Progenitor for the Type IIb SN 2024abfo
Authors: Zexi Niu, 泽茜 牛, Ning-Chen Sun, Justyn R. Maund, Zhen Guo, Wenxiong Li, Meng Sun, 萌 孙, Jifeng Liu
Figure caption: The PSF subtraction of images obtained in 2018 December as an example. Each row shows single-exposure images before (left) and after (right) the PSF subtraction. Red and cyan scatters mark the fitted positions of the SN progenitor candidate and Source B, respectively. In the g and r bands, to avoid contamination from Source B (cyan), we performed PSF fitting for Source B and the progenitor candidate simultaneously. In the z band of all epochs, Source B was undetected in the single-exposure image; therefore, PSF photometry was only performed for the progenitor candidate. Projections centered at the progenitor candidate along the x- and y-axis are also shown for each panel. The progenitor and Source B are successfully subtracted, and no visible residuals remain in the subtracted images.
Paper: Discovery of a Variable Yellow Supergiant Progenitor for the Type IIb SN 2024abfo
Authors: Zexi Niu, 泽茜 牛, Ning-Chen Sun, Justyn R. Maund, Zhen Guo, Wenxiong Li, Meng Sun, 萌 孙, Jifeng Liu
Figure caption: An example of the zero-point fitting for the PSF photometry of DECaLS single-exposure images. The left-hand panel plots the zero-point measurements (red vertical line) for the g-band image taken in 2018, where gray and black points represent data before and after a 3σ clipping, respectively. The right-hand panel shows the distribution of absolute values of residuals, where the blue line indicates the rms of different instrumental magnitudes. Near the progenitor candidate’s magnitude (indicated by the red dashed line), the rms of the residuals is approximately 0.17 mag.
Paper: Discovery of a Variable Yellow Supergiant Progenitor for the Type IIb SN 2024abfo
Authors: Zexi Niu, 泽茜 牛, Ning-Chen Sun, Justyn R. Maund, Zhen Guo, Wenxiong Li, Meng Sun, 萌 孙, Jifeng Liu
Figure caption: The evolution of positions on the HR diagram for the progenitor candidate, with different assumed circumstellar reddenings. Different epochs (yyyy-mm) are marked with different colors in the same way as in Figure 6. For reference, BPASS single star evolution tracks (metallicity; Z = 0.01; J. J. Eldridge et al. 2017) are also plotted with different initial masses. Well-constrained progenitors of SN IIb 1993J, SN 2011dh, SN 2013df, SN 2016gkg, and SN 2017gkk are plotted in light blue. The derived effective temperatures and bolometric luminosities are listed in Table 3.
Paper: Discovery of a Variable Yellow Supergiant Progenitor for the Type IIb SN 2024abfo
Authors: Zexi Niu, 泽茜 牛, Ning-Chen Sun, Justyn R. Maund, Zhen Guo, Wenxiong Li, Meng Sun, 萌 孙, Jifeng Liu
Figure caption: Light curves of PSF photometry for the progenitor candidate in the g-, r-, and z-band images from 2013 to 2018. The deduced explosion date of the SN is 2024 November 14 (MJD 60628; A. Reguitti et al. 2025). The hatched regions denote the weighted mean values of the photometry in 2013 December and their corresponding uncertainties.
Paper: Discovery of a Variable Yellow Supergiant Progenitor for the Type IIb SN 2024abfo
Authors: Zexi Niu, 泽茜 牛, Ning-Chen Sun, Justyn R. Maund, Zhen Guo, Wenxiong Li, Meng Sun, 萌 孙, Jifeng Liu
Figure caption: SEDs of the progenitor candidate at different epochs. The vertical error bars represent 1σ uncertainty, and the gray shaded regions indicate the bandpasses of the g, r and z bands. The best-fitting stellar atmospheric models with no circumstellar extinction are plotted in the same color as the data points for different epochs.
Paper: Discovery of a Variable Yellow Supergiant Progenitor for the Type IIb SN 2024abfo
Authors: Zexi Niu, 泽茜 牛, Ning-Chen Sun, Justyn R. Maund, Zhen Guo, Wenxiong Li, Meng Sun, 萌 孙, Jifeng Liu
Figure caption: An example of the uncertainties in differential astrometry for DECaLS images. The pixel size of DECaLS images is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩262.
Paper: A Relativistic Jet in the Radio-quiet Active Galactic Nucleus Mrk 110
Authors: Ailing Wang, Tao An, Kenneth I. Kellermann, Hua Feng, Emmanuel K. Bempong-Manful, Roland Timmerman, Shaoguang Guo
Figure caption: Radio observations of Mrk 110. (a) VLBA 6.2 GHz images of Mrk 110 from 2021 December 31 (color scale) and 2024 February 2 (contours), showing a core shift of ∼1.6 mas. The image center is set at the 2021 December peak position (R.A. = 09:25:12.84781, decl. = +52:17:10.3862). (b) International LOFAR image at 144 MHz observed on 2016 August 16, revealing a ∼1.7 kpc northern extension aligned with the parsec-scale jet. (c) Peak position evolution. (d) Change of the radio spectrum from 2015 to 2024, showing transformation from a steep (α = −0.76) to inverted (α = +0.69) spectral index. Historical data (2015–2016) are from F. Panessa et al. (2022); our recent measurements are detailed in Table 1. Dashed lines indicate power-law fits.
Paper: A Relativistic Jet in the Radio-quiet Active Galactic Nucleus Mrk 110
Authors: Ailing Wang, Tao An, Kenneth I. Kellermann, Hua Feng, Emmanuel K. Bempong-Manful, Roland Timmerman, Shaoguang Guo
Figure caption: VLBI images of Mrk 110 are presented, with the observation date, peak intensity, and rms noise level indicated in the bottom left corner of each map. The contour levels are 3 × rms × (1, 2, 4, 8, 16) mJy beam–1. The position of the Gaia DR3 optical nucleus (Gaia Collaboration 2022) is marked by a plus sign at the center of each panel. The gray ellipse in the bottom right corner illustrates the restoring beam’s shape.
Paper: A Relativistic Jet in the Radio-quiet Active Galactic Nucleus Mrk 110
Authors: Ailing Wang, Tao An, Kenneth I. Kellermann, Hua Feng, Emmanuel K. Bempong-Manful, Roland Timmerman, Shaoguang Guo
Figure caption: Proper motion of the radio core in Mrk 110 at 7.6 GHz derived from VLBA observations between 2021 and 2024. The top, middle, and bottom panels show the evolution of ΔR.A., Δdecl., and total displacement ΔR (in milliarcseconds), respectively, as a function of observation date. Two distinct motion phases are identified: an earlier phase from 2021 to 2023 (red dashed–dotted lines) and a later phase from 2023 to 2024 (red dotted lines).
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Multiwavelength time series and evolution of optical and radio polarization properties from IXPE, Swift, VLT, and VLA collected on 2024 June 4–5. Error bars represent 1σ c.l. (uncertainties in the fourth panel are smaller than markers). In panels five and six, red horizontal lines show the average optical polarization degree (Popt) and angle (PAopt), with shaded areas indicating ±1σ. In the eighth panel, the dotted line marks a flat spectrum. In the ninth panel, downward arrows indicate 3σ upper limits on the radio polarization fraction (Pradio).
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Protractor plot of X-ray polarization degree and angle for the high mode, derived from a weighted spectro-polarimetric analysis, compared with the optical polarization angle. The polarization degree and angle are measured over the energy ranges 2–6, 2–3, and 3–6 keV, and are displayed along the radial and azimuthal directions, respectively. Contours represent 90% confidence regions. The black dashed line and gray shaded area indicate the optical R-band polarization angle and its 90% c.l. uncertainty.
Paper: Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe
Authors: Michael J. West, Roberto De Propris, Maret Einasto, Z. L. Wen, J. L. Han
Figure caption: Alignments of galaxy clusters in the WH24 sample as a function of comoving separation (d) and their evolution with the redshift (z). The statistic ﹩\langle \cos (2\theta )\rangle ﹩ measures the strength of cluster alignments, with an expectation value of 0 if cluster orientations are uncorrelated. Error bars indicate the standard error of the mean for each bin. The orange curve is a best-fit exponential function for each redshift bin; the amplitude (α) and decay scale (τ) of the best-fit components are listed in Table 1. The red dots are the results from each of 1000 Monte Carlo simulations in which each cluster was assigned a random orientation, destroying any intrinsic alignments that might be present in the data. The insets show an expanded view for the largest separations. Statistically significant alignments are found over separations up to 200–300 cMpc in all but the highest redshift subsample.
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Top panel: time evolution of optical intensity (red) and of the Qopt (brown) and Uopt (orange) Stokes parameters. Bottom panel: scatter plot of Stokes parameters for the optical emission from J1023. Data points are color-coded based on the time of their measurements, with a diamond marker highlighting the epoch corresponding to the low mode detected during simultaneous X-ray observations. BMJD stands for Barycentric Modified Julian Date. TDB indicates the Barycentric Dynamical Time.
Paper: Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe
Authors: Michael J. West, Roberto De Propris, Maret Einasto, Z. L. Wen, J. L. Han
Figure caption: Top: a number density plot of the sky distribution of 1.58 million clusters in the Z. L. Wen & J. L. Han (2024) catalog. Bottom left: the redshift distribution of the clusters. Bottom right: the number of detected member galaxies in each cluster as a function of redshift. For reference, 1° on the sky subtends roughly 60 cMpc at redshift z = 1.
Paper: Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe
Authors: Michael J. West, Roberto De Propris, Maret Einasto, Z. L. Wen, J. L. Han
Figure caption: The Perseus–Pisces supercluster region is a nearby segment of the cosmic web. Each point in this figure represents a galaxy in NASA’s Extragalactic Database with a recessional velocity in the range 4000–9000 km s−1, corresponding to distances of ∼150–300 million lt-yr from Earth. Densely populated groups and clusters of galaxies dot the prominent filament like beads on a string. The major axis orientations of two of these clusters, A426 and A262, are shown.
Paper: Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe
Authors: Michael J. West, Roberto De Propris, Maret Einasto, Z. L. Wen, J. L. Han
Figure caption: Cluster alignments at four different redshifts in the LastJourney simulation. As in Figure 4, the red dots are the results from 1000 Monte Carlo simulations in which each cluster was assigned a random orientation. The insets show an expanded view for the largest separations. Statistically significant alignments are found in the simulations for separations up to 200–300 cMpc in all but the highest redshift clusters.
Paper: Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe
Authors: Michael J. West, Roberto De Propris, Maret Einasto, Z. L. Wen, J. L. Han
Figure caption: Dependence of alignments on cluster mass (left) and ellipticity (right) for all redshifts combined. Note that in some cases the error bars are smaller than the symbol size. The most massive and most elongated clusters are the most strongly aligned with their neighbors. The data are plotted logarithmically to facilitate comparison.
Paper: Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe
Authors: Michael J. West, Roberto De Propris, Maret Einasto, Z. L. Wen, J. L. Han
Figure caption: Projected particle distribution in three typical LastJourney clusters at redshift z = 0. The major axis orientation for each, determined from the moments of inertia of its particle distribution, is shown in red. Coordinates are relative to the cluster center.
Paper: Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe
Authors: Michael J. West, Roberto De Propris, Maret Einasto, Z. L. Wen, J. L. Han
Figure caption: Cluster member galaxies in a 2° × 2° portion of the WH24 catalog. Each point represents an individual galaxy. The different colors correspond to different redshift bins: blue is for z < 0.4, green is for z = 0.4–0.7, orange indicates z = 0.7–1, and red is for z > 1.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Custom atmospheric models generated with PICASO to fit the JWST NIRCam F444W and MIRI F1140C photometric detections of C6, along with the 3σ upper limit in F200W and the 5σ upper limits in the H2 and H3 filters from SPHERE. All models assume a surface gravity of log(g) = 2.75 (cgs), with the object’s mass (∼0.3 MJup) varying slightly to maintain this surface gravity and the corresponding radius. The best-fitting models within the 1σ uncertainty correspond to 325 K planets with 10 × solar metallicity. The C/O ratio and radius can vary to match the observed photometry. The two insets provide a detailed look at each photometric detection.