adsabs/AstroCLIMB huggingface dataset:
Paper: CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts
Authors: G. Yang, 光 杨, K. I. Caputi, C. Papovich, P. Arrabal Haro, M. B. Bagley, P. Behroozi, E. F. Bell, L. Bisigello, V. Buat, D. Burgarella, Y. Cheng, N. J. Cleri, R. Davé, M. Dickinson, D. Elbaz, H. C. Ferguson, S. L. Finkelstein, N. A. Grogin, N. P. Hathi, M. Hirschmann, B. W. Holwerda, M. Huertas-Company, T. A. Hutchison, E. Iani, J. S. Kartaltepe, A. Kirkpatrick, D. D. Kocevski, A. M. Koekemoer, V. Kokorev, R. L. Larson, R. A. Lucas, P. G. Pérez-González, P. Rinaldi, L. Shen, J. R. Trump, A. de la Vega, L. Y. A. Yung, J. A. Zavala
Figure caption: Left: SED-fit examples from CIGALE. The object in the top/middle/bottom panel is classified as SF/mixed/AGN. Within each panel, the top subpanel displays the data points and the best-fit SED models (i.e., flux density vs. observed wavelength). The purple and red data points indicate the observed and model flux densities, respectively. The black curves represent the total model SEDs. The red and orange curves indicate the galactic dust and AGN components, respectively. The blue/yellow curves represent unattenuated/attenuated stellar. The fitted redshift and fracAGN are labeled. The bottom subpanel displays the relative residual in the flux, i.e., (observed−model)/observed. Right: the corresponding 5″ × 5″ cutouts from HST/F160W and MIRI.
Paper: CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts
Authors: G. Yang, 光 杨, K. I. Caputi, C. Papovich, P. Arrabal Haro, M. B. Bagley, P. Behroozi, E. F. Bell, L. Bisigello, V. Buat, D. Burgarella, Y. Cheng, N. J. Cleri, R. Davé, M. Dickinson, D. Elbaz, H. C. Ferguson, S. L. Finkelstein, N. A. Grogin, N. P. Hathi, M. Hirschmann, B. W. Holwerda, M. Huertas-Company, T. A. Hutchison, E. Iani, J. S. Kartaltepe, A. Kirkpatrick, D. D. Kocevski, A. M. Koekemoer, V. Kokorev, R. L. Larson, R. A. Lucas, P. G. Pérez-González, P. Rinaldi, L. Shen, J. R. Trump, A. de la Vega, L. Y. A. Yung, J. A. Zavala
Figure caption: Photometric redshift distribution of our MIRI sources. The blue, orange, and red bars represent SF, mixed, and AGN types, respectively. The inset panel zooms in on the z ≳ 3 part of the histogram.
Paper: JWST/NIRSpec Measurements of the Relationships between Nebular Emission-line Ratios and Stellar Mass at z ∼ 3–6
Authors: Alice E. Shapley, Naveen A. Reddy, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer
Figure caption: Nitrogen-related emission-line ratios vs. stellar mass for CEERS galaxies. These panels show the line ratios [N II] λ6583/Hα (left), O3N2 (middle), and [N II] λ6583/[O II] λ3727 (right) vs. M *. All of these ratios include the [N II] λ6583 feature commonly used to probe ISM conditions at z ≤ 2.5. In each panel, the background grayscale histogram corresponds to the distribution of local SDSS star-forming galaxies. Individual CEERS galaxies are color-coded as in Figure 1 and indicated as small squares for detections or downward-facing (upward-facing) arrows for upper (lower) limits. Measurements from stacked CEERS spectra are indicated as large circles with the same color-coding as individual measurements. Measurements from stacked spectra of galaxies in the MOSDEF survey at z ∼ 1.5 (Topping et al. 2021) and z ∼ 2.3 (Sanders et al. 2021) are shown, respectively, with large gold and red triangles. In the right panel ([N II] λ6583/[O II] λ3727), we overplot low-mass galaxies from the LVL survey (Berg et al. 2012) with small cyan symbols, in order to indicate the regime of primary nitrogen enrichment in which N/O is independent of metallicity.
Paper: JWST/NIRSpec Measurements of the Relationships between Nebular Emission-line Ratios and Stellar Mass at z ∼ 3–6
Authors: Alice E. Shapley, Naveen A. Reddy, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer
Figure caption:  α-related emission-line ratios vs. stellar mass for CEERS galaxies. The panels show the line ratios [O III] λ5007 (top left), O32 (top right), R23 (bottom left), and [Ne III] λ3869/[O II] λ3727 (bottom right). Symbols are as in Figure 3. In addition, measurements from stacked spectra of galaxies in the MOSDEF survey at z ∼ 3.3 (Sanders et al. 2021) are shown with large green triangles.
Paper: JWST/NIRSpec Measurements of the Relationships between Nebular Emission-line Ratios and Stellar Mass at z ∼ 3–6
Authors: Alice E. Shapley, Naveen A. Reddy, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer
Figure caption: Stellar mass vs. redshift for all 94 CEERS galaxies at 2.7 ≤ z ≤ 6.5 analyzed in this work. Galaxies at z = 2.7–4.0 are color-coded green; those at z = 4.0–5.0 are shown in blue; finally, those at z = 5.0–6.5 are indicated in magenta.
Paper: JWST/NIRSpec Measurements of the Relationships between Nebular Emission-line Ratios and Stellar Mass at z ∼ 3–6
Authors: Alice E. Shapley, Naveen A. Reddy, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer
Figure caption: Composite spectrum of the high-mass bin of CEERS galaxies at z = 4.0–5.0. The composite spectrum is indicated with a black curve, while the error spectrum is shown in red. In the top row, the full composite spectrum is shown, along with the mean redshift and stellar mass. The bottom row includes three zoomed-in regions covering the vicinity of the key nebular lines analyzed in this work. These emission lines are labeled and marked with vertical dotted lines in both full and zoomed-in spectral panels.
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: Planetary and stellar parameters for systems with λ measurements (left) and the subset of systems with ψ measurements (right). In the top and bottom rows, the color of the data points conveys the planet’s orbital separation and mass, respectively. Triangular data points are members of the λ sample, i.e., λ has been measured but not ψ. Circular data points are for the ψ sample, i.e., both λ and ψ have been measured.
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: The isonormal distribution used in Model 2 for different choices of w.
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: Biases in the ﹩v\sin i﹩ method (Section 7.3) and the gravity-darkening method (Section 7.4) shape the recovered obliquity distribution. Each panel shows the obliquity distribution of hypothetical stars drawn from a randomly oriented population, after applying increasingly stringent detection thresholds. Left: obliquities measured with the ﹩v\sin i﹩ method, using three detection thresholds: (i) ﹩v\sin i\gt 2\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, (ii) photometric amplitude A > 0.7%, where ﹩A={f}_{\mathrm{spot}}\sin i﹩, and (iii) A > 0.9%. The ﹩v\sin i﹩ method favors ψ = 0° and 180°. Right: obliquities measured with the gravity-darkening method. The detection thresholds were parameterized by the difference in reduced χ 2 between modeling the light curve with gravity-darkening or a standard transit profile.
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: The λ measurements from the ψ sample are slightly but systematically higher than the λ measurements from the λ sample. This effect is likely due at least in part to the selection bias of the gravity-darkening method, which was used in five cases in the ψ sample and no cases in the λ sample. In each panel, the λ measurements are plotted from lowest to highest, with blue points for the λ sample and purple points for the ψ sample. The left panel shows all available measurements. The center panel omits data from the gravity-darkening method. The right panel is for the weak-tides sample. For each measurement, the 1σ uncertainty interval is plotted as a vertical line.
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: Inferred obliquity distributions for different samples and likelihoods. Regardless of the sample, the peak in the isonormal model is small enough to be consistent or nearly consistent with the isotropic model. Left: the ψ sample of 72 planets for which measurements of both λ and i ⋆ are available, analyzed with the ψ likelihoods. Center: the λ sample of 102 planets, analyzed with the λ likelihoods. Right: the entire ψ and λ sample of 174 planets, analyzed with the ψ and λ likelihoods. Solid lines demarcate the mean, and the shaded regions show the 1σ uncertainty intervals.
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: The distribution of achievable measurement precision in λ for the nominal system described in the text, assuming random stellar orientations and either a fixed impact parameter or a uniform distribution of impact parameters. The median value of σ  λ  is presented as a solid line, and the shaded regions demarcate the 1σ and 2σ percentiles. Color indicates the assumed radial velocity measurement uncertainty: 1 m s−1 (blue) or 5 m s−1 (gold).
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: Observational investment required to recover a peaked obliquity distribution, for three idealized campaigns: (i) measuring λ only, (ii) measuring ﹩\sin i﹩ only, and (iii) measuring both λ and ﹩\sin i﹩. The vertical axis is the fraction of realizations in which the postulated peak (see Section 8) is successfully identified. In the left panel, the horizontal axis is the sample size; in the right panel, the horizontal axis is the total observing time, assuming 5 hr per λ measurement and 0.25 hr per ﹩v\sin i﹩ measurement.
Paper: Ponderings on the Possible Preponderance of Perpendicular Planets
Authors: Jared C. Siegel, Joshua N. Winn, Simon H. Albrecht
Figure caption: Projected-obliquity (left) and full-obliquity (right) vs. stellar effective temperature. Blue points represent planets for which λ has been measured but not ψ. Purple points represent planets for which ψ has been measured. Circles are the giant-planet hosts in the weak-tides sample, triangles are the gravity-darkening measurements, and crosses are all other measurements.
Paper: Eruption of a Magnetic Flux Rope in a Comprehensive Radiative Magnetohydrodynamic Simulation of Flare-productive Active Regions
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Magnetic field of the source region of the eruption. (a): Line-of-sight magnetic field (B  z ) in the photosphere (surface of optical depth of unity). The red box indicates the source active region of the flare. (b): B  z  in the source region. Arrows show the vector of the horizontal magnetic field. (c): Angles between the actual magnetic field (full vector) and the potential field in the photosphere. (d): Magnetic field lines above the PIL. Field lines are calculated from seed points that are randomly distributed above the PIL. Seed points for the blue lines spread between z = 9.4 and 14 Mm, and seed points for the red lines are in height range between z = 2.8 and 7.5 Mm. Golden lines are calculated from seed points distributed between z = 1.0 and 2.5 Mm. (e): The same field lines from a horizontal view.
Paper: Eruption of a Magnetic Flux Rope in a Comprehensive Radiative Magnetohydrodynamic Simulation of Flare-productive Active Regions
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Magnetic field and plasma thermal properties in a vertical cut (y–z plane) at x = 87 Mm. (a): B  x . Arrows show the direction of the magnetic field in the plane (B  y  and B  z ). (b): Magnetic twist integrated along field lines (evaluated for each grid point above z = 0.5 km). (c) and (d): Plasma temperature and density in the same vertical cut. Panels (a)–(d) and (e)–(f) present the same quantities for two snapshots, respectively.
Paper: GRB 191019A: A Short Gamma-Ray Burst in Disguise from the Disk of an Active Galactic Nucleus
Authors: Davide Lazzati, Rosalba Perna, Benjamin P. Gompertz, Andrew J. Levan
Figure caption: Best-fit model for the prompt light curve of GRB 191019A. Neil Gehrels Swift Observatory data (blue symbols) are adapted from Levan et al. (2023). The thick orange line shows the best-fit model for the overall prompt light curve. The thin green line marks the photospheric component, while the thin red line displays the contribution of the strong reverse shocks driven into the fireball by the dense external medium.
Paper: GRB 191019A: A Short Gamma-Ray Burst in Disguise from the Disk of an Active Galactic Nucleus
Authors: Davide Lazzati, Rosalba Perna, Benjamin P. Gompertz, Andrew J. Levan
Figure caption: Monte Carlo Markov Chain parameter estimation for the prompt light curve of GRB 191019A. All parameters are well constrained, with the exception of the electron fraction Y  e , which only shows a mild preference for small values.
Paper: Rotation Reduces Convective Mixing in Jupiter and Other Gas Giants
Authors: J. R. Fuentes, Evan H. Anders, Andrew Cumming, Bradley W. Hindman
Figure caption: Horizontally averaged profiles of composition ﹩\overline{C}﹩, convective composition flux ﹩\overline{{wC}}﹩, and the kinetic energy flux in the vertical direction ﹩(1/2)\overline{w{{\boldsymbol{u}}}^{2}}﹩ (left, middle, and right panel, respectively). The overline denotes that variables are averaged over the horizontal directions. Note that  u  2 = u 2 + v 2 +  w 2 , where u, v, and w are the x, y, and z components of the velocity. The results are shown at a time where the convection boundary is located at z = 0.75 (i.e., h = 1.25) for both runs. This time corresponds to t = 3750 for the nonrotating case and t = 11500 for the rotating case. The background colors distinguish between the convection zone and the stable region.
Paper: Rotation Reduces Convective Mixing in Jupiter and Other Gas Giants
Authors: J. R. Fuentes, Evan H. Anders, Andrew Cumming, Bradley W. Hindman
Figure caption: Panel (a): thickness of the convection zone h as a function of time t. The results are shown for both the rotating and nonrotating cases. The solid lines correspond to the best fits of the form ﹩h(t)={[{h}_{0}^{1/n}+K(t-{t}_{0})]}^{n}﹩ for each case. We obtain n ≈ 0.49 for the nonrotating case (compared to the analytic prediction n = 0.5) and n ≈ 0.40 for the rotating case (compared to the analytic prediction n = 5/12 ≈ 0.41). See Section 4 for more details. Panel (b): Rosim, ﹩{\mathrm{Ro}}_{\mathrm{sim}}^{1/2}﹩, and F  K,R/F  K,NR as a function of the thickness of the convection zone, h. Note that ﹩{\mathrm{Ro}}_{\mathrm{sim}}^{1/2}﹩ has similar values to F  K,R/F  K,NR, giving support to Equation (4).
Paper: Rotation Reduces Convective Mixing in Jupiter and Other Gas Giants
Authors: J. R. Fuentes, Evan H. Anders, Andrew Cumming, Bradley W. Hindman
Figure caption: Volume renderings of the z component of the vorticity  ω  = ∇ ×  u  for the nonrotating case (left) and rotating case (right). For both cases, the snapshots are shown at times when the bottom of the convection zone has expanded beyond the initial location (from z = 1 to 0.75). The Rossby number in the rotating case is ﹩{\mathrm{Ro}}_{\mathrm{sim}}\approx 0.065﹩, computed using the averaged flow velocity in the convection zone, and thickness of the convection zone.
Paper: Atomic Hydrogen Scaling Relations at z ≈ 0.35
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: The M HI−M * scaling relation, based on measurements of 〈MHI〉 in blue star-forming galaxies. The blue filled circles show our H I 21 cm stacking measurements of ﹩\mathrm{log}\,\langle {{\rm{M}}}_{{\rm{H}}{\rm\small{I}}}\rangle /{{\rm{M}}}_{\odot }﹩ in three (logarithmic) stellar-mass bins for blue galaxies at z ∼ 0.35 in the EGS. The solid blue line is the best-fit mean M HI−M * scaling relation, with the light blue shaded region showing the 68% confidence interval around the fit. The figure also shows the mean M HI−M * scaling relations for blue star-forming galaxies at (1) z ≈ 0 from the xGASS sample (as a dashed line; Catinella et al. 2018), (2) z ≈ 1 from the GMRT-CATz1 survey (as a dotted line; Chowdhury et al. 2022a), and (3) at z ≈ 0.37 from the MIGHTEE survey (as a dashed–dotted line; Sinigaglia et al. 2022). Note that all scaling relations in the panel have been obtained by fitting a relation to the dependence of ﹩\mathrm{log}\ \langle {{\rm{M}}}_{{\rm{H}}{\rm\small{I}}}\rangle ﹩ on M *, and not to ﹩\langle \mathrm{log}\ {{\rm{M}}}_{{\rm{H}}{\rm\small{I}}}\rangle ﹩, as is usually done at z ≈ 0 (e.g., Catinella et al. 2018).
Paper: Atomic Hydrogen Scaling Relations at z ≈ 0.35
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: The characteristic H I depletion timescale as a function of stellar mass at different redshifts. The blue circles show the measurements of the characteristic H I depletion times for blue galaxies at z ≈ 0.35 for three stellar-mass bins, while the blue solid line and shaded region show, respectively, the t dep−M * scaling relation and the 68% confidence interval for these galaxies. The figure also shows the characteristic H I depletion timescales for blue star-forming galaxies at (1) z ≈ 0 from the xGASS sample (dashed line; Catinella et al. 2018), (2) z ≈ 1 from the GMRT-CATz1 survey (dotted line; Chowdhury et al. 2022a), and (3) z ≈ 0.37 from the MIGHTEE-HI survey (dashed–dotted line; Sinigaglia et al. 2022). Note that all scaling relations in the panel have been obtained uniformly by combining the ﹩\mathrm{log}\ \langle {M}_{{\rm{H}}{\rm\small{I}}}\rangle -\mathrm{log}\ {M}_{* }﹩ relation with the (redshift-dependent) main-sequence relation from Whitaker et al. (2012).
Paper: Atomic Hydrogen Scaling Relations at z ≈ 0.35
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: The stacked H I 21 cm emission spectra (in units of luminosity density) for blue galaxies in three (logarithmic) stellar-mass bins, (A) ﹩8.00\leqslant \mathrm{log}\ ({M}_{* }/{M}_{\odot })\lt 8.70﹩, (B) ﹩8.70\leqslant \mathrm{log}\ ({M}_{* }/{M}_{\odot })\lt 9.45﹩, and (C) ﹩9.45\leqslant \mathrm{log}\ ({M}_{* }/{M}_{\odot })\leqslant 10.40﹩. The dashed black curves in each panel show the rms noise in the corresponding velocity planes of the stacked spectral cubes. See the text for discussion.
Paper: Origin and Extent of the Opacity Challenge for Atmospheric Retrievals of WASP-39 b
Authors: Prajwal Niraula, Julien de Wit, Iouli E. Gordon, Robert J. Hargreaves, Clara Sousa-Silva
Figure caption: An overview of the limitations of spectral line parameter for CO2. (a) The sparse data for the CO2–H2 system. Here, experimentally measured half-widths (Hanson & Whitty 2014; Padmanabhan et al. 2014) do not provide sufficient coverage for populating the HITRAN database (Gordon et al. 2022). The CO2-air-broadening parameters in HITRAN have therefore been scaled to the measurement of Hanson & Whitty (2014) to retain rotational structure (Tan et al. 2022), even though rotational dependence is not expected to be exactly the same. (b) The effect of temperature dependence. A demonstration of the combined effect of using the CO2–H2 and CO2-air parameters (i.e., γ and n) for a typical P(40) transition in HITRAN. In this example, the relative difference increases at higher temperatures. (c) Limitations of the Voigt profile regarding the far-wing behavior of CO2 lines. Experimental absorption of the 4.3 μm at 25°C in 1 atm N2 (PNNL; Sharpe et al. 2004) compared to modeled spectra that use HITRAN2020 parameters with different line wing cutoffs that are typically used for Earth (Mlawer et al. 2012) and exoplanetary atmospheres (Amundsen et al. 2014; Chubb et al. 2021; Gharib-Nezhad et al. 2021). The approximate experimental sensitivity is shown as the dashed line.
Paper: Origin and Extent of the Opacity Challenge for Atmospheric Retrievals of WASP-39 b
Authors: Prajwal Niraula, Julien de Wit, Iouli E. Gordon, Robert J. Hargreaves, Clara Sousa-Silva
Figure caption: Left: Comparison of carbon dioxide 4.3 μm feature closest to the temperature of 900 K and 1 atm pressure for the five opacity models used in our study. The different opacity models are offset for the purpose of clarity. Top right: Comparison of models at the observational resolution of NIRSpec/G395H generated for WASP-39 b using five different cross sections using mass of 0.28 M Jup, P 0 1.0 atm, T 0 900.0 K, Log MR﹩{}_{{\mathrm{CH}}_{4}}﹩ −5.0, Log MRCO −10.0, LogMR﹩{}_{{\mathrm{CO}}_{2}}﹩ −2.0, Log MR﹩{}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ -1.0, Log MR﹩{}_{{{\rm{H}}}_{2}{\rm{S}}}﹩ −4.0, LogMR﹩{}_{\mathrm{HCN}}﹩ −4.0, and Log MR﹩{}_{{\mathrm{SO}}_{2}}﹩ −4.0. Bottom right: The observed deviations obtained from the inter-model comparisons. The transmission model using CS-H2-25 was used as the base model for comparison.
Paper: Origin and Extent of the Opacity Challenge for Atmospheric Retrievals of WASP-39 b
Authors: Prajwal Niraula, Julien de Wit, Iouli E. Gordon, Robert J. Hargreaves, Clara Sousa-Silva
Figure caption: Left: the change of SSD with temperature and the size of the planet with five JWST transits with the same observational noise and abundance as WASP-39 b. We assume the planet mass follows the relationship from Chen & Kipping (2017) and the transit depth at the probed pressure corresponds to 1%. The region where atmospheres are hydrodynamically unstable has been left blank. Middle: the same plot but 10% abundance of the metallicity seen in WASP-39 b. Right: the same plot but 1% abundance of the metallicity seen in WASP-39 b.
Paper: Origin and Extent of the Opacity Challenge for Atmospheric Retrievals of WASP-39 b
Authors: Prajwal Niraula, Julien de Wit, Iouli E. Gordon, Robert J. Hargreaves, Clara Sousa-Silva
Figure caption:  p–T profile for five different cross-section retrievals constructed and the corresponding 1σ confidence interval. The contribution function as a function of pressure is also shown with axis going from right to left. The dotted lines along the y-axis show the pressure levels most probed for the present observations of WASP-39 b. The two synthetic cases from N22 are shown in dashed lines—a super-Earth (green), and a warm Jupiter (black)—meanwhile, the Earth is shown in dashed red.
Paper: Origin and Extent of the Opacity Challenge for Atmospheric Retrievals of WASP-39 b
Authors: Prajwal Niraula, Julien de Wit, Iouli E. Gordon, Robert J. Hargreaves, Clara Sousa-Silva
Figure caption: Posterior distribution of the retrieved parameters retained for WASP-39 b for NIRSpec G395H for the isothermal (solid) and parametric (dotted) p–T atmospheric model. The posteriors of the parameters are tabulated in Table 1. The scatter among the different retrievals when using different cross sections is inherently larger than the observed precision for different molecules. The rightmost panel of the bottom row shows carbon to oxygen ratio calculated from the retrieved carbon and oxygen bearing molecular species.
Paper: Origin and Extent of the Opacity Challenge for Atmospheric Retrievals of WASP-39 b
Authors: Prajwal Niraula, Julien de Wit, Iouli E. Gordon, Robert J. Hargreaves, Clara Sousa-Silva
Figure caption: Best fit showing different molecules using the results from the CS-H2-25 cross sections. The isothermal model yields ﹩{\chi }_{\nu }^{2}﹩ of 1.08 showing the adequacy of the current model to explain the trends observed in the data.