adsabs/AstroCLIMB huggingface dataset:
Paper: RIOJA. JWST and ALMA Unveil the Inhomogeneous and Complex Interstellar Medium Structure in a Star-forming Galaxy at z = 6.81
Authors: Mitsutaka Usui, Ken Mawatari, Javier Álvarez-Márquez, Takuya Hashimoto, Yuma Sugahara, Rui Marques-Chaves, Akio K. Inoue, Luis Colina, Santiago Arribas, Carmen Blanco-Prieto, Yurina Nakazato, Naoki Yoshida, Tom J. L. C. Bakx, Daniel Ceverino, Luca Costantin, Alejandro Crespo Gómez, Masato Hagimoto, Hiroshi Matsuo, Wataru Osone, Yi W. Ren, Yoshinobu Fudamoto, Takeshi Hashigaya, Miguel Pereira-Santaella, Yoichi Tamura
Figure caption: Redshift evolution of the electron density ne. The red star indicates the electron density of COS-2987, derived from the [O II] ratio. Literature data at z ∼ 0–3 are compiled from R. L. Sanders et al. (2016; [S II] or [O II]) and R. L. Davies et al. (2021; [S II]), while data at z ≳ 4 are taken from Y. Isobe et al. (2023), Abdurro’uf et al. (2024), and C. Marconcini et al. (2024), all based on the [O II] ratios. The filled symbols represent measurements for individual galaxies, and the open symbols represent median values for the sample galaxies. The electron density of COS-2987, derived from the [O II] ratio, is consistent with the overall redshift evolution trend indicated by the blue dashed line (Abdurro’uf et al. 2024).
Paper: RIOJA. JWST and ALMA Unveil the Inhomogeneous and Complex Interstellar Medium Structure in a Star-forming Galaxy at z = 6.81
Authors: Mitsutaka Usui, Ken Mawatari, Javier Álvarez-Márquez, Takuya Hashimoto, Yuma Sugahara, Rui Marques-Chaves, Akio K. Inoue, Luis Colina, Santiago Arribas, Carmen Blanco-Prieto, Yurina Nakazato, Naoki Yoshida, Tom J. L. C. Bakx, Daniel Ceverino, Luca Costantin, Alejandro Crespo Gómez, Masato Hagimoto, Hiroshi Matsuo, Wataru Osone, Yi W. Ren, Yoshinobu Fudamoto, Takeshi Hashigaya, Miguel Pereira-Santaella, Yoichi Tamura
Figure caption: Radial profiles of the [O III] 5008 and [O III] 88 emission lines. The blue and red lines represent the profiles of [O III] 5008 and [O III] 88, respectively, with the shaded regions indicating their corresponding uncertainties.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: (a) Combined MIRI F770W (blue), F1130W (green), and F2100W (red) images of II Zw 40. The originally core-saturated MIRI images were recovered using the methods detailed in Section 3. The box indicates the NIRSpec footprint. (b) Spectral extraction regions used throughout this Letter. The map is generated by stacking the cube between 3.25 and 3.34 μm. The dashed black circle shows the aperture for total extraction, while orange and blue solid circles represent areas used to extract the SSC-N and SSC-S PAH spectra, respectively, as shown in Figure 3. Our grid extraction, centered on the northern SSC, yielded eight complete NIRSpec+MIRI/MRS spectra spanning 2.9–24.5 μm used for resolving PAH properties in II Zw 40, with corresponding cell numbers indicated.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: (a) Combined NIRSpec and MIRI IFU spectrum of II Zw 40, extracted from a 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩6 radius aperture (dashed black circle in Figure 1(b)), showing strong fine-structure and recombination lines along with weak H2 and PAH features. The three detected PAH bands are highlighted, with other key diagnostics labeled. For comparison, the lower-resolution (R ∼ 120) AKARI+Spitzer spectrum is shown as a dotted line, scaled by 4× for clarity. (b)–(d) Continuum-subtracted zoom-ins of the PAH bands at 3.3, 6.2, and 11.3 μm, with dashed profiles representing the 1C PAH template for star-forming galaxies from T. S. Y. Lai et al. (2020), normalized to the 3.3 μm band strength. In II Zw 40, the weaker 6 and 11 μm bands relative to the template indicate a shift in PAH power toward the 3.3 μm feature.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: The left panels display results from II Zw 40, while the right panels provide context by comparing them to other star-forming regions in NGC 7469 (T. S. Y. Lai et al. 2023) and photodissociation regions in the Orion Bar. The Orion Bar data include the H II and diffuse front (DF3) from R. Chown et al. (2024) and E. Peeters et al. (2024). Red points denote individual cell results, with the purple star showing the total extraction. Results from both SSC-N and SSC-S are also shown; overall, the different extractions exhibit a consistent trend. A red shaded region illustrates the propagated limit for ratios involving ΣPAH, with the orange solid line indicating the midpoint of our possible distribution (see Section 5.1.1 for more details). Panels (a) and (b) demonstrate that PAH emission becomes increasingly suppressed relative to ionizing neon emission as radiation fields harden. Panel (c) shows the decrease of the fractional 3.3 μm PAH power with respect to the neon ratio as the galaxy is resolved. Panel (d) reveals that PAH emission is heavily suppressed in II Zw 40, with ΣPAH-to-neon ratios ∼100 times lower than those in NGC 7469’s star-forming ring and ∼10 times lower than the Orion Bar. However, as shown in panel (e), PAH 3.3 suppression is slightly less severe, decreasing only about 60× compared to NGC 7469. Panel (f) illustrates how this nonuniform suppression of PAHs and greater retention of 3.3 μm emission leads to the enhancement of the fractional PAH 3.3 strength. Based on the conservative midpoint distribution, this enhancement can reach ∼10%—at least twice the level observed in reference star-forming regions, underscoring the notable shift of PAH power toward the 3.3 μm PAH in II Zw 40.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: The 3.3 μm PAH emission in II Zw 40. The two II Zw 40 spectra, extracted from the apertures outlined in Figure 1(b), represent the SSC-N (orange) and SSC-S (blue) regions. The CAFE fits to the 3.3 μm PAH feature and nearby lines and continuum in II Zw 40 are shown, with the PAH 3.3 bands shown in shaded purple. The 3.47 μm plateau feature can be seen in SSC-S. Also shown is the starburst template spectrum from NGC 7469 in T. S. Y. Lai et al. (2023). Notably, II Zw 40 displays a significantly different relative flux ratio between the 3.3 μm PAH band and the Pfδ line compared to typical star-forming galaxies, with the Pfδ emission being exceptionally strong. For better visibility, the spectra of SSC-S and the starburst ring in NGC 7469 are scaled as indicated.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: (Top panel) The comparison between the 3.3 μm PAH flux based on the continuum subtraction method using the three NIRSpec midband filters and the result from spectral decomposition. Each point is color-coded by the fractional contribution of the 3.3 μm PAH to the combined PAH and Pfδ emission. The red line represents the T. S. Y. Lai et al. (2020) photometric PAH 3.3 empirical relationship, which aligns well with regions where PAH emission dominates over the Pfδ line. The inset demonstrates the relative positions of the filters and the derived synthetic photometry with respect to the spectrum from the total extraction shown in Figure 2. (Bottom panel) The division between the spectroscopically measured PAH 3.3 and the empirical relationship from the top panel. The x-axis is expressed in surface brightness. Based on the binning results (in red), the photometric method can recover the “true” 3.3 μm PAH flux within 50% when the continuum-subtracted F335M surface brightness exceeds 0.1 MJy sr−1.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: High spatial resolution maps from NIRSpec, with a pixel size of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩05 and a typical PSF of ∼0﹩\mathop{.}\limits^{^{\prime\prime} }﹩19 at 3.3 μm. (a) A map of the 3.3 μm emission, highlighting the two main SSCs in II Zw 40, indicated by the plus signs. (b) and (c) Spectral decomposition reveals two distinct components. (b) The 3.3 μm PAH map, uncovering its elongated morphology not visible in (a). Overlaid CO (3–2) contours from ALMA (S. M. Consiglio et al. 2016) indicate cospatiality with 3.3 μm PAH, while yellow contours represent the [Ne III]/[Ne II] ratio. The offset between the 3.3 μm PAH emission and neon ratio is intriguing, resembling blisters found at the edges of H II regions. (c) The Pfδ map, shown alongside an Hα gray-scale map from HST, where the Hα contour closely aligns with Pfδ, suggesting a strong correlation. (d) The Pfδ/PAH 3.3 ratio map, overlaid with the PAH 3.3 contour from (b), shows a peak displaced from the 3.3 μm PAH emission, highlighting the spatial offset between PAH 3.3 and Pfδ.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: PAH (and aliphatic) band ratios plotted against [Ne III]/[Ne II], which probes radiation field hardness. Different symbols represent various band ratios as shown in the legend. Only the PAH 3.3/11.3 ratio exhibits a significant correlation (r = −0.92), with a 1σ spread of ∼0.06 dex (shaded), suggesting larger average PAH sizes in regions with harder radiation fields. Other band ratios show no significant variations.
Paper: Resolving Emission from Small Dust Grains in the Blue Compact Dwarf II Zw 40 with JWST
Authors: Thomas S.-Y. Lai, 劭愉 賴, Sara Duval, J. D. T. Smith, Lee Armus, Adolf N. Witt, Karin Sandstrom, Elizabeth Tarantino, Shunsuke Baba, Alberto Bolatto, Grant P. Donnelly, Brandon S. Hensley, Masatoshi Imanishi, Laura Lenkic, Sean Linden, Takao Nakagawa, Henrik W. W. Spoon, Aditya Togi, Cory M. Whitcomb
Figure caption: A zoom-in view of the IFU total extraction shown in Figure 2, focusing on the 7.7 and 17 μm ranges to demonstrate the nondetection of PAH emission at 7.7, 8.6, and 17 μm. Red dashed curves represent the scaled starburst template from T. S. Y. Lai et al. (2020), provided as a reference to illustrate typical PAH profiles in these spectral regions.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: Panel (a) demonstrates that the BZ mechanism accurately describes the outflow power for arbitrary non-Kerr BHs out to large horizon angular frequencies beyond even extremal Kerr BHs. This implies that the BZ power is a fundamental property of spinning BHs. The red shaded region indicates the predicted BZ power over a range of magnetic field shapes: 0.044 ≤ k ≤ 0.054 from Equation (1). Panel (b) shows that the outflow power can assume a large range of values given a particular BH spin within our model set. Panel (c) is similar to panel (b) but presents the deviation in mean BH shadow diameter with respect to the Schwarzschild value of ﹩{d}_{{\rm{sh}},{\rm{Schw}}}=6\sqrt{3}\,M﹩, hereafter δ ﹩:= ﹩ dsh/dsh,Schw − 1. We also show the 2017 EHT measurements of M87* of δ = −0.01 ± 0.17 (K. Akiyama et al. 2019; D. Psaltis et al. 2020; P. Kocherlakota et al. 2021), delineated as dashed lines. These plots illustrate the inherent degeneracies in BH spin inference from jet power estimates and shadow image size measurements when one relaxes the assumption that the spacetime geometry is described by a Kerr BH. See Section 4 for more discussion on these degeneracies.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: Top panel: snapshot 3D rendering of a BH accreting gas and launching magnetized jets (GRMHD simulations of a JP BH with α22 = 2 and a = 0.9; see Section 2), together with a zoomed-in view of the vicinity of the event horizon (inset). The diffuse material comprising the large-scale relativistic jet is shown in blue, with the extended denser accretion disk material shown in red and yellow. The tightly wound magnetic field within the jet and counterjet is indicated by the gray lines, with the BH event horizon denoted by the central dark sphere. Bottom panel: corresponding ray-traced GRRT image of the upper panel’s GRMHD snapshot as viewed at 86 GHz (logarithmic color scale), together with the inset zoomed-in view of the event horizon-scale structure, as viewed at the Event Horizon Telescope (EHT) frequency of 230 GHz (linear color scale) for M87*.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: Collection of four square panels of three-image groups: the 86 GHz M87* images (upper sub-panel) and corresponding 230 GHz BH shadow images (both viewed at i = 163°, bottom left) and as viewed at i = 90° (bottom right), with the header indicating the BH model. From left to right, top to bottom, trios of sub-panels represent Schwarzschild BH, Kerr BH with a = 0.5, JP BH with α13 = 6 and a = 0.5, and a JP BH with α22 = 8 and a = 0.5, respectively. Differences in jet size and power are evident between Schwarzschild and Kerr BHs at 86 GHz. The JP BH with α13 = 6, in spite of having the same spin as the Kerr BH, has a significantly weaker jet and larger photon ring size. By contrast, the JP BH with α22 = 8 possesses a large ΩH, enhancing the effects of frame dragging, giving rise to a more powerful and extended jet than the Kerr BH with identical spin. All panels show time-averaged images over the interval 20,000–25,000 M. The 86 GHz image color scale is logarithmic and spans 5 orders of magnitude in specific intensity, whereas the 230 GHz images are plotted on a linear scale and show the full range of specific intensity. All images are normalized to a maximum pixel intensity of unity.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: Breaking degeneracies in BH parameters. Left: the outflow power η depends strongly on the horizon angular frequency ΩH for the Kerr and non-Kerr JP α22 models. η increases monotonically as ∣ΩH∣ increases both for prograde and retrograde BHs. Therefore, it is possible to constrain ∣ΩH∣ using measurements of the outflow efficiency from observations of jetted BHs. Right: contours of ΩH (in color) overlaid with contours of the shadow size deviation δ for JP α22 spacetimes. Independent measurements of ΩH and δ could place stringent constraints on the BH spin a and quadrupole moment α22. Forbidden solutions for the JP metric are shown by the gray-striped region.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: Time evolution of the accretion rate ﹩\dot{M}﹩, the outflow power P, the square of the unnormalized horizon magnetic flux ﹩{{\rm{\Phi }}}_{{\rm{H}}}^{2}﹩ (which is essentially equivalent to the expected BZ power) and the 230 GHz flux for four different (non-)Kerr models. We also mention the ratio of the 1σ standard deviation and the mean μ for each curve as a measurement of the variability of each quantity for each model.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: We find that the instantaneous outflow efficiencies from all models and their individual time snapshots fall in line with the BZ prediction. The inset shows the same figure but zoomed in to a smaller range in ΩHϕH. Figure 2(a) shows the time-averaged η instead.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: Accretion rate normalized horizon magnetic flux ϕH for our model set as a function of the corresponding horizon angular frequency ΩH. We find that there is an approximate cubic dependence on ΩH, with the largest deviations seen in the non-Kerr α13 models.
Paper: On the Universality of Energy Extraction from Black Hole Spacetimes
Authors: Koushik Chatterjee, Ziri Younsi, Prashant Kocherlakota, Ramesh Narayan
Figure caption: Jet shape profiles for four models with jets. The horizon angular frequency ΩH and the jet efficiency η both increase as one moves from Model A through to D. It is found that the jet becomes increasingly more collimated as its power increases.
Paper: Dynamo Confinement of a Radiatively Spreading Solar Tachocline Revealed by Self-consistent Global Simulations
Authors: Loren I. Matilsky, Lydia Korre, Nicholas H. Brummell
Figure caption: Dots: realized amplitude of ∣Bpol∣2 in the RZ summed over the largest scales (m = 0, 1, 2), where m is the azimuthal wavenumber. Solid curve: profile for ∣Bpol∣2 predicted by the nonaxisymmetric, quasi-cyclic skin effect. The skin-predicted amplitude comes from summing the exponential damping profiles ≈﹩\exp (2({r}_{{\rm{c}}}-r)/{\delta }^{m\omega })﹩ over all ω and m = 0, 1, 2, weighted by the value of ﹩| {{\boldsymbol{B}}}_{{\rm{pol}}}^{m\omega }{| }^{2}﹩ at the interface r = rc. Both profiles are normalized to 1 at r = rc. For full details, see M24’s Equations (21)–(23).
Paper: Dynamo Confinement of a Radiatively Spreading Solar Tachocline Revealed by Self-consistent Global Simulations
Authors: Loren I. Matilsky, Lydia Korre, Nicholas H. Brummell
Figure caption: Simulated equatorially symmetric component of the differential rotation ﹩{\left\langle {\rm{\Omega }}\right\rangle }_{t}/{{\rm{\Omega }}}_{0}-1﹩, in (a) the HD case and (b) the MHD case. The color bars are normalized separately for positive and negative values and the contour ﹩{\left\langle {\rm{\Omega }}\right\rangle }_{t}\equiv {{\rm{\Omega }}}_{0}﹩ is dashed.
Paper: Dynamo Confinement of a Radiatively Spreading Solar Tachocline Revealed by Self-consistent Global Simulations
Authors: Loren I. Matilsky, Lydia Korre, Nicholas H. Brummell
Figure caption: Nondimensional azimuthally and temporally averaged equatorially symmetric components of the torque densities, radially averaged for r/R⊙ < 0.696 (i.e., below the approximate base of the overshoot layer), shown for (a) the HD case and (b) the MHD case. See M24’s Equation (17) for the full definitions of the torque densities marked in the legend.
Paper: Dynamo Confinement of a Radiatively Spreading Solar Tachocline Revealed by Self-consistent Global Simulations
Authors: Loren I. Matilsky, Lydia Korre, Nicholas H. Brummell
Figure caption: Three-dimensional spherical cutout showing a snapshot of the simulated flows (﹩{\omega }_{z}^{{\prime} }﹩ for r > rc) and fields (Bθ for r < rc) in the MHD case. The spherical surfaces are close to the boundaries and the meridional surfaces are located 90° apart. Each radial level is normalized separately by the rms of the appropriate quantity at that level.
Paper: Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems
Authors: Howard Chen, Matthew S. Clement, Le “Chris” Wang, Jesse T. Gu
Figure caption: Time series of VGS-calculated atmospheric water, shallow mantle water, and planetary mass growth for TRAPPIST-1 c and d analogs. Atmospheric water and shallow mantle water are in units of Earth's ocean mass and planetary mass is in units of Earth mass. Solid blue lines indicate the median values, with shaded regions representing the 20th–75th percentile range. Light, thin curves represent five randomly selected individual runs. In both planets, the inclusion of a luminous pre-main sequence (PMS) phase (left panels) strongly suppresses atmospheric water growth compared to PMS-free cases (right panels), with final water contents differing by up to a factor of three. This suppression is most pronounced in the inner planet (TRAPPIST-1 c), where PMS heating limits early volatile retention. Shallow mantle water is shown only for PMS-free scenarios, as PMS-driven volatile loss prevents substantial mantle hydration in the PMS-included runs.
Paper: Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems
Authors: Howard Chen, Matthew S. Clement, Le “Chris” Wang, Jesse T. Gu
Figure caption: Time series of VGS-simulated surface-to-mantle volatile mass ratios for example simulations of TRAPPIST-1 b ((a), (b), (c), and (d)) and TRAPPIST-1 e ((e), (f), (g), and (h)). The panels are H2O wet planetesimal ((a) and (e)), CO2 wet planetesimal ((b) and (f)), H2O dry planetesimal ((c) and (g)), and CO2 dry planetesimal ((d) and (h)). Refer to Section 2 regarding how the water mass fractions are set in our model.
Paper: Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems
Authors: Howard Chen, Matthew S. Clement, Le “Chris” Wang, Jesse T. Gu
Figure caption: Final surface CO2 (left) and N2 (right) masses (in units of Earth’s total carbon and nitrogen reservoir) of each planet as a function of total planet mass (in units of M⊕) and orbital distance (in au). The water mass fractions of accreted planetesimals and embryos are assumed to follow the stepwise function given by Equations (1)–(3). Measured TRAPPIST-1 properties are indicated by black circles (E. Agol et al. 2021).