adsabs/AstroCLIMB huggingface dataset:
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Escape fraction, fesc, as a function of the redshift. The blue hatched box shows the 1σ ranges, fesc = ﹩1{4}_{-7}^{+9} \% ﹩, and the dotted line shows the best fit, fesc = 12%, for the stars. The red hatched box shows the 1σ ranges, fesc = ﹩6{0}_{-32}^{+28} \% ﹩, and the line shows the best fit, fesc = 63%, for the AGN. Observational constraints and 1σ uncertainties of fesc for star-forming galaxies from C. C. Steidel et al. (2018), A. J. Pahl et al. (2021), A. Saldana-Lopez et al. (2022), R. Begley et al. (2022), S. Mascia et al. (2023), and C. Cain et al. (2025) are shown as indicated. 1σ upper limits of fesc for star-forming galaxies from M. J. Rutkowski et al. (2016), J. Matthee et al. (2017), and X. Wang et al. (2025) are shown with down-facing arrows. Light red data points with error bars are from B. M. Smith et al. (2020, 2024) and A. Grazian et al. (2018) and show results and 1σ uncertainties of fesc for AGN. The gray line shows the closed-box metallicity history on the right-side vertical axis.
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Top: ionizing efficiency, ξion, as a function of the redshift. The black line shows the ξion obtained from the median CSFH and CAGNH for the hybrid model, while the blue and red lines show the same for the stellar and AGN contributions. The dashed gray line shows the canonical value, ﹩{\mathrm{log}}_{10}({\xi }_{{\rm{ion}}})=25.2﹩, from B. E. Robertson et al. (2013). The dotted purple/green line and filled regions show the linear fits and 1σ uncertainties from C. Simmonds et al. (2024a, 2024b), where we are extrapolating at z > 9. Triangle points with error bars show the results and 1σ uncertainties from R. Jaiswar et al. (2024). Bottom: CSED from the PROSPECT model computed at z = 6. The black line shows the total SED obtained from the median CSFH and CAGNH, while the blue and red lines show the SED for the stars and AGN. The gray dotted and dashed lines show the total SEDs at z = 2 and z = 12. The vertical line shows the Lyman limit, λ = 912 Å, and the vertical band shows the top-hat filter of Δλ = 100 Å centered on 1500 Å for the UV.
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Top: ﹩{\dot{n}}_{{\rm{ion}}}(z)﹩ as a function of the redshift. The black hatched region is the result of the hybrid model, as in Figure 6. We show with filled regions the 1σ spread of the models from C. A. Mason et al. (2019b) in pink, S. L. Finkelstein et al. (2019) in dark blue, and R. J. Bouwens et al. (2015a) in light blue. The three different reionization models: ES/EE, ES/LE, and LS/LE from C. Cain et al. (2025) are shown with blue, purple, and red dashed lines. Bottom: neutral fraction as a function of the redshift. The filled regions and dashed lines have the same meaning as the top panel. The cyan line is the JWST-ξion model from J. B. Muñoz et al. (2024). We also show with green lines the results from the THESAN-I (R. Kannan et al. 2022) and the MERAXES (S. Balu et al. 2023) simulations.
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Neutral fraction as a function of the redshift using the same fesc for both stars and AGN found in the previous section. The hatched and filled regions show the results for ﹩{ \mathcal C }=3,12,30﹩ as indicated in the legend. The width of the regions corresponds to the 1σ uncertainties from the CSFH and CAGNH (as in Figure 6). The dashed lines are from F. B. Davies et al. (2024) corresponding to ﹩{ \mathcal C }=3,12﹩ as indicated. F. B. Davies et al. (2024) assumed that ﹩{\mathrm{log}}_{10}({f}_{{\rm{esc}}}\,{\xi }_{{\rm{ion}}})=24.8﹩ (see Equation (1)), which is why their curves are generally shifted to the right in comparison to ours.
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: fesc as a function of ﹩{ \mathcal C }﹩. The blue hatched region shows the 1σ ranges, and the circle shows the best fit for the stars. The red hatched region and circle show the 1σ ranges and best fit for the AGN. The filled shaded regions show the 2σ ranges with the same color scheme as above.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: Observational data used in this work. Left panel: SED. Photometry in colored markers and Spitzer/InfraRed Spectrograph (IRS) spectrum (N. J. Evans et al. 2003, 2009) in magenta. A combined BT-settl stellar photosphere spectrum (F. Allard et al. 2003, 2011) with a 8500 K blackbody radiation fitting the UV data point and another blackbody radiation with 1500 K from the radius of R⋆ to 0.055 au represent the accreting gas disk at the inner edge, shown as a gray line. Right panels: ALMA band 6 continuum (240 GHz) radial profile from DSHARP (S. M. Andrews et al. 2018) and C18O (2–1) radial profile (lower right) and disk-integrated line profile (lower left) from MAPS (K. I. Öberg et al. 2021). The disk-integrated line profile is compiled from GoFish (https://github.com/richteague/gofish) (R. Teague 2019), and the radial profiles are measured at each radius with an elliptical annulus with the inclination and position angles in the continuum image and the C18O moment-0 maps, respectively. SED references: UV photometry from Swift (L. I. Cleeves et al. 2016); optical photometry from APASS (A. A. Henden et al. 2016), Gaia (Gaia Collaboration et al. 2023), and D. L. Padgett et al. (2006); infrared photometry from 2MASS (M. F. Skrutskie et al. 2006), WISE (E. L. Wright et al. 2010), Spitzer (D. L. Padgett et al. 2006), and AKARI (D. Ishihara et al. 2010); and (sub)millimeter data from C. Pinte et al. (2008), S. M. Andrews et al. (2018), K. I. Öberg et al. (2011), L. I. Cleeves et al. (2017), J. Huang et al. (2017), DSHARP (J. Huang et al. 2018), L. I. Cleeves et al. (2016), and D. Lommen et al. (2008).
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The synthetic SED compared with observation (top) and the synthetic ﹩{L}_{{{\rm{C}}}^{18}{\rm{O}}(2-1)}﹩ for different Mgas compared with an observation (bottom) for the well-mixed model. In the top panel, the observations are shown in black points with errors, the Spitzer/IRS spectrum is shown with the magenta line, and the input stellar spectra with the stellar photosphere, UV, as well as the inner gas disk are shown with the dashed gray line. The synthetic SED of the model is shown with the orange line, with the inferred Mdust shown on the upper right corner. In the bottom panel, the black horizontal line shows the C18O(2–1) observation from MAPS, with its uncertainties shown as the dark gray area. The blue points show the model points with different ε, and the best-fit model with ε = 6.41 × 10−3 is circled in blue, with its corresponding Mgas shown on the upper right corner.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: Flow chart summarizing the two approaches to estimate disk masses. The main difference between them is the surface density distributions of gas and dust. We solve vertical hydrostatic equilibrium (VHSE) for all models and include dust settling for the structured model (see Sections 3.2 and 3.3), and we use the reduced chemical network that considers the isotope-selective photodissociation and grain surface chemistry to get the CO abundances. This flow chart only shows the main steps in DiskMINT, and more details are described in D. Deng et al. (2023).
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: Mgas estimates in the literature. From left to right, they include Mgas based on Mdust multiplied by a constant ISM gas-to-dust mass ratio of 100 from P+08 (C. Pinte et al. 2008), C+16 (L. I. Cleeves et al. 2016), Z+21 (K. Zhang et al. 2021), the dynamical Mgas by L+23 and M+24 (G. Lodato et al. 2023; P. Martire et al. 2024), the Mgas inferred from the 12CO-emitting height by P+25 (T. Paneque-Carreño et al. 2025), and the Mgas inferred from the CO isotopologue line fluxes by Z+21 (K. Zhang et al. 2021), T+25 (L. Trapman et al. 2025a), and this work. The solid pentagons and circles represent models with no assumed CO or C depletion, and the hollow ones are derived with a depletion factor that is annotated alongside. The dotted black horizontal line shows the median value of the derived dynamical mass, with the shaded gray region showing its uncertainty. Mgas is better constrained by recent works: L. Trapman et al. (2025a) used a combination of 13CO, C18O & N2H+ line emission, and this work utilizes C18O line emission only. Both works find Mgas estimates that are consistent with the inferred dynamical Mgas within quoted uncertainties. For the estimates obtained in this work, the lower and upper limits are marked as ×0.75 and ×2, respectively, and are shown as dashed error bars because they represent the uncertainties associated with the method, rather than the statistical errors quoted for the points in the literature.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The gas surface densities for the well-mixed (orange), structured (blue), and dust dynamics test scenario (green) are shown in the top panel. The dotted lines represent the regions where we lack observational information to derive robust results, including the inner disk, where it becomes optically thick (vertical dashed line) and the outer disk that is beyond measured dust or gas radii (Rdust and Rgas shown in vertical dashed–dotted lines). In the bottom panel, the three lines show Σdust(r) for different grain sizes when computed using fragmentation and drift: green line for all grain sizes, blue dashed line for larger grains (a ≥ adrift) that have drifted in, and magenta dashed–dotted line for smaller grains (a < adrift). There are some visible steps in the dust surface densities in both panels, and they are due to the effect of the dust fragmentation solved from a finite number of dust size bins.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The dust continuum radial distribution with different ufrag (top) and Σdust(r) (bottom) for the model with ufrag = 500 cm s−1. The models presented here are with fragmentation-dominated grain size distributions, and we do not include the dust drifting. In the top panel, we plot the observed continuum radial distribution in black with its uncertainties in gray, and the models with ufrag = 1000, 750, 500, 100 cm s−1 are shown in blue, green, orange, and brown, respectively. In the bottom panel, the Σdust(r) for all dust grains, large grains (a ≥ 0.005 cm, which is responsible for the millimeter-wavelength continuum emission), and small grains (a < 0.005 cm) are shown as black solid, blue dashed, and pink dashed–dotted lines, respectively. The gray vertical dashed line marks the region where the dust becomes optically thick, and the gray vertical dashed–dotted line shows the dust outer radius Rdust.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: Comparison of observations and the results from structured model, in SED (top), continuum and C18O(2–1) radial profiles (middle two panels), and C18O(2–1) line spectra (bottom). The captions in the SED follow the top panel of Figure 3, with the synthetic SED from the structured model shown in blue. The continuum and C18O(2–1) radial profiles are created by measuring the total flux per area at each radius inside an annulus that is tilted to match the observed geometry, with the best-fit Mdust and Mgas shown at the upper right corners. The line spectra are made with GoFish without deprojection. Observations are shown in black lines, along with their uncertainties, in the radial profile and the line spectra.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The flow chart demonstrates the steps to calculate dust settling when solving the vertical density distribution. The details on the procedures of solving thermal equilibrium and the VHSE are presented in D. Deng et al. (2023) Section 2.1 and Figure 1. For all models, the well-mixed case where dust is coupled with gas and the structured model where they decouple due to settling, the same convergence criterion is used—that ρgas and ρdust attain a 5% accuracy with iterations.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The maximum size (﹩{a}_{{\rm{\max }}}﹩) that the dust grain could live as limited by the drift (black solid line) or fragmentation (color dashed lines). The ﹩{a}_{{\rm{\max }}}﹩ at different radii are constrained by the smaller value solved from either drift or fragmentation (with a certain ufrag), and they are solved based on the surface density and the thermal profile for the validation model. The fragmentation is always the dominant size-constraining factor in the inner disk and could also dominate in the outer disk if ufrag < 750 cm s−1. Drift could only become the dominant factor at the outer disk with relatively large ufrag ≳ 750 cm s−1.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The dust-to-gas surface density ratio for the structured model, with the Stokes number at the disk midplane for the 0.1 cm grains shown at the top axis. We show the total surface densities in blue, the surface densities that are only up to one pressure scale height (1 h) in orange, and the average of the two lines in red dotted–dashed lines. We also show the dust gaps and rings identified in C. J. Law et al. (2021) in dotted and solid vertical black lines, respectively.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: Comparison of SED (top), dust continuum and C18O(2–1) radial profile (middle), and C18O(2–1) line spectra between the dust dynamics test model and observation. All notations are the same as in Figure 5, with the green lines representing the model result and the black line showing the observation with uncertainties shaded by the gray area.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: Flow chart summarizing the steps for the theoretical test of dust dynamics.
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Transmission spectrum of TOI-270 d. Gold squares with error bars show the observed JWST spectrum from B. Benneke et al. (2024). The pink and blue lines show forward modeled spectra assuming the upper atmospheric composition from our coupled magma–atmosphere model. Model parameters are Tm−a = 3000 K, Tc−m = 4000 K, xFe = 33%, and Kzz = 107 cm2 s−1. The pink line shows a case where nitrogen is enhanced in line with the carbon and oxygen enhancement found by the magma–atmosphere model. The blue line shows a case where nitrogen is depleted to 10−2 × solar abundance, in line with expectations of nitrogen depletion from magma–atmosphere interactions (O. Shorttle et al. 2024). For the model with enhanced nitrogen, χ2/ndata = 1.31, and for the model with depleted nitrogen, χ2/ndata = 1.18.
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Volume mixing ratio profiles for chemical species in the atmosphere of TOI-270 d, based on interactions between a magma ocean and a gaseous atmosphere with an initial solar composition. Model parameters are Tm−a = 3000 K, Tc−m = 4000 K, xFe = 33%, and Kzz = 107 cm2 s−1. The bottom panel shows volume mixing ratios of species at the mantle–atmosphere interface (P ≫ 100 bar). Error bars and arrows show measured volume mixing ratios or upper limits for H2O; CH4 and CO2; and CO and NH3 in the upper atmosphere, derived from JWST observations of TOI-270 d (B. Benneke et al. 2024). Dashed lines show nitrogen-bearing chemical species not included in the magma ocean model, but included in the upper atmosphere model. In the case shown here, atmospheric nitrogen is depleted to 10−2 × solar.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Plasma parameters shown on a meridional slice through the active region. The first column is at t = 0 minute, the second at t = 30 minutes, and the third at t = 60 minutes post-eruption. The first row shows electron density, the second row shows electron temperature, the third row shows proton temperature, and the fourth row shows magnetic field strength. The white lines represent the magnetic field lines in the flux rope and surrounding corona.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: The top panel shows the magnetic (blue), kinetic (red), thermal (black), and absolute value of the gravitational potential (purple) energies, and the total energy (gray) integrated over the SC domain for the first 6 hr. The bottom panel shows the radiative (pink) and heat conduction (green) cooling rates and the Alfvén wave heating rate (orange) integrated over the SC domain, over the first 6 hr. In both panels, the background corona is subtracted.
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Volume mixing ratios of CO (green, solid) and CO2 (red, dashed) in the upper atmosphere of TOI-270 d (P = 1 mbar) as a function of Kzz. Tm−a = 3000 K, Tc−m = 4000 K, and xFe = 33% for all models shown here. The red shaded region shows the constraints on the volume mixing ratio of CO2 reported by B. Benneke et al. (2024), and the green dotted line shows the reported 2σ upper limit for CO.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Energetic quantities shown on a meridional slice through the active region. The first column is at t = 0 minute, the second at t = 30 minutes, and the third at t = 60 minutes post-eruption. The first row shows the absolute value of the gravitational potential energy density (GPE), the second row shows the kinetic energy density (KE), the third row shows the thermal energy density (ETH), and the fourth row shows the magnetic energy density (ME). The white lines represent the magnetic field lines in the flux rope and surrounding corona.
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Volume mixing ratio profiles for NH3 and HCN for a range of initial atmospheric nitrogen abundances. Model parameters are Tm−a = 3000 K, Tc−m = 4000 K, xFe = 33%, and Kzz = 107 cm2 s−1. The 188 × solar case represents nitrogen enhancement in line with the derived metallicity from the resulting carbon and oxygen abundances from the magma–atmosphere model. The arrow represents the 2σ upper limit for the NH3 volume mixing ratio according to B. Benneke et al. (2024).