adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Detection of [O III] 88 μm at z = 12.33: Exploring the Nature and Evolution of GHZ2 as a Massive Compact Stellar System
Authors: Jorge A. Zavala, Tom Bakx, Ikki Mitsuhashi, Marco Castellano, Antonello Calabro, Hollis Akins, Veronique Buat, Caitlin M. Casey, David Fernandez-Arenas, Maximilien Franco, Adriano Fontana, Bunyo Hatsukade, Luis C. Ho, Ryota Ikeda, Jeyhan Kartaltepe, Anton M. Koekemoer, Jed McKinney, Lorenzo Napolitano, Pablo G. Pérez-González, Paola Santini, Stephen Serjeant, Elena Terlevich, Roberto Terlevich, L. Y. Aaron Yung
Figure caption:  ALMA Band 8 spectrum covering the [O III] 52 μm transition at z ≈ 12.3. Analog to Figure 1 but for the 52 μm observations. The left panel shows a 3.″5 × 3.″5 image of the collapsed data cube within the expected FWHM of the line (based on the [O III] 88 μm detection). Nevertheless, there is no significant detection around the position of GHZ2 (black cross). Contours show ±1σ and ±2σ, with dashed lines for negative values. The extracted spectrum at the position of the source is shown on the right panel along with the redshift constraints from the different instruments.
Paper: [C II] Properties and Far-infrared Variability of a z = 7 Blazar
Authors: Eduardo Bañados, Yana Khusanova, Roberto Decarli, Emmanuel Momjian, Fabian Walter, Thomas Connor, Christopher L. Carilli, Chiara Mazzucchelli, Sofía Rojas-Ruiz, Bram P. Venemans
Figure caption: ALMA and NOEMA observations of J0410–0139. Top: continuum-subtracted [C II] spectrum, extracted from a 1.″5 radius aperture (yellow circle in the next panel). The red line is a Gaussian fit to the data (a second Gaussian can be fitted at ∼300 km s−1, but we found this not to be statistically significant; see Section 3.1). The [C II] measured properties, luminosity, and SFR are listed in Table 1. The [C II] line is not detected in the NOEMA data. Middle: ALMA [C II] (left) and continuum (right) maps. The beam size for these observations is 0.″49 × 0.″68. The [C II] map is the average over 247 km s −1 (1.2× FWHM of the spectrum shown in the top panel). The yellow circle is the 1.″5 radius aperture centered on the [C II] centroid (yellow cross) used to extract the [C II] spectrum. Bottom: NOEMA continuum maps at 224 (left) and 239 (right) GHz, with beam sizes 0.″78 × 1.″63 (left) and 0.″72 × 1.″53 (right). The source is unresolved in the NOEMA observations. The optical position of the quasar is shown with a white cross on each panel, which is consistent with the peak of the ALMA and NOEMA continuum, but the peak of the [C II] map is offset by 0.″35 (yellow cross in [C II] map). All contour plots are shown at ±[3, 5, 10, 20, 30]σ (dashed contours represent negative values). The σ for each map is at the top-left corner of each panel.
Paper: [C II] Properties and Far-infrared Variability of a z = 7 Blazar
Authors: Eduardo Bañados, Yana Khusanova, Roberto Decarli, Emmanuel Momjian, Fabian Walter, Thomas Connor, Christopher L. Carilli, Chiara Mazzucchelli, Sofía Rojas-Ruiz, Bram P. Venemans
Figure caption: SED in the radio and (sub)millimeter regime of J0410–0139. The data points are color coded by year of observation for visualization purposes. Only the observations taken at a similar epoch in 2021 and 2022 are shown (see Figure 2 in E. Bañados et al. 2024 for the full SED and other epochs). The VLA 2021 and 2022 observations were taken in the same observing block, yielding a quasi-simultaneous view of the SED (within 15 minutes in the rest frame). The VLA 2021 and NOEMA observations are taken 6.5 days apart in the source’s rest frame, while the VLA 2022 and ALMA observations are 2.8 days apart. The dashed lines are power-law extrapolations from the VLA low- and high-frequency measurements. The pentagons and star show the NOEMA and ALMA measurements, respectively (see also Figure 1). The ∼238 GHz continuum decreased by ∼33% from the NOEMA 2021 to ALMA 2022 measurements. The VLA flux densities above 3 GHz decreased on average by ∼37% from 2021 to 2022 (see Section 3.2), strongly suggesting that the differences between the NOEMA and ALMA data are due to the variability of the synchrotron emission. In contrast, we show models of modified blackbody emission (with typical dust temperatures of T d = 47 K and emissivity index of β = 1.6) with the colored curves. By failing to account for the IR contribution of the synchrotron emission, single-epoch measurements of cold gas in the host galaxy would be very different and incorrect.
Paper: [C II] Properties and Far-infrared Variability of a z = 7 Blazar
Authors: Eduardo Bañados, Yana Khusanova, Roberto Decarli, Emmanuel Momjian, Fabian Walter, Thomas Connor, Christopher L. Carilli, Chiara Mazzucchelli, Sofía Rojas-Ruiz, Bram P. Venemans
Figure caption: Ratio of [C II] to IR luminosities (8–1000 μm) vs. IR luminosities. The local galaxies and the high-redshift sources that are not quasars are compiled as in E. Bañados et al. (2015), including data from S. Malhotra et al. (2001) and I. De Looze et al. (2014). The z > 5.7 radio-quiet quasars are from B. P. Venemans et al. (2020), M. L. Luhman et al. (2003), T. Díaz-Santos et al. (2013), and F. Wang et al. (2024). The FIR (42.5−122.5 μm) luminosities from B. P. Venemans et al. (2020) are converted as L TIR = 1.41 × L FIR. The z > 5.7 radio-loud quasars are from Y. Khusanova et al. (2022) and E. Bañados et al. (2023). The open circles are sources undetected in both [C II] and IR continuum. The red star and blue pentagon correspond to the properties of J0410–0139 using the IR properties derived from NOEMA in 2021 and ALMA in 2022, respectively. At face value, these measurements would place J0410–0139 as the lowest data point in L [C II]/L IR among the z > 5.7 quasars. However, we argue that the IR luminosity is contaminated by synchrotron emission, as evidenced by variability. The open star and pentagons show the location of J0410–0139, consistent with local (U)LIRGs, if we require that the SFR derived from IR luminosity matches the one derived from the [C II] line. In this case, the measured IR luminosity is dominated by synchrotron radiation: ∼85% in 2021 and ∼80% in 2022.
Paper: Tracing Back a Second-generation Star Stripped from Terzan 5 by the Galactic Bar
Authors: Stefano O. Souza, Marica Valentini, Cristina Chiappini, Angeles Pérez-Villegas, Josefina Montalbán, Diego Bossini, Beatriz Barbuy, Yvonne Elsworth, Rafael A. Garcia
Figure caption: Chemodynamical properties of SOS1. (a) X–Y and X–Z density projections of the Galaxy with the orbit of SOS1 star (red line). (b) Abundances of and light elements for SOS1 (yellow star symbol) compared with field stars in the inner Galaxy (density plot). (c) The left panel shows the Jacobi energy of the GCs compatible within 1σ with SOS1 (shaded yellow region), and the right panel shows the SOS1 distance to the center of the selected clusters.
Paper: Tracing Back a Second-generation Star Stripped from Terzan 5 by the Galactic Bar
Authors: Stefano O. Souza, Marica Valentini, Cristina Chiappini, Angeles Pérez-Villegas, Josefina Montalbán, Diego Bossini, Beatriz Barbuy, Yvonne Elsworth, Rafael A. Garcia
Figure caption: Dissociation time calculation. The gray histogram shows the distribution of lookback time obtained from the dissociation points. The black solid line shows the multiple Gaussian distribution obtained through the GMM fitting, and the individual Gaussians are as black thin dashed lines. The two significant dissociation times τd1 and τd2 are highlighted as red and yellow lines, respectively. The number above each Gaussian represents the individual contribution to the total fitting. The inset plot shows the AIC test.
Paper: [C II] Properties and Far-infrared Variability of a z = 7 Blazar
Authors: Eduardo Bañados, Yana Khusanova, Roberto Decarli, Emmanuel Momjian, Fabian Walter, Thomas Connor, Christopher L. Carilli, Chiara Mazzucchelli, Sofía Rojas-Ruiz, Bram P. Venemans
Figure caption: The 40 km s−1 [C II] channel maps of the continuum-subtracted data of J0410–0139. Solid (dashed) contours correspond to positive (negative) values starting at 2σ with steps of 1σ, where σ is the noise in each individual channel. The synthesized beam is shown in the lower-left corner of each panel.
Paper: Black Hole Scaling Relations in the Dwarf-galaxy Regime with Gaia-Sausage/Enceladus and ωCentauri
Authors: Guilherme Limberg
Figure caption: MBH–M⋆. Local (z ∼ 0) regular (non-AGN) galaxies are shown as blue and orange diamonds for late- and early-type galaxies, respectively (J. E. Greene et al. 2020). White triangles with black edges are constraining MBH upper limits derived from stellar dynamics (also compiled by J. E. Greene et al. 2020), including Fornax dSph (Fnx; J. R. Jardel & K. Gebhardt 2012). MW is in yellow (R. Genzel et al. 2010). Local AGNs are shown as the gray plus signs (A. E. Reines & M. Volonteri 2015). Green pentagons show a compilation of dwarf AGNs (also by A. E. Reines & M. Volonteri 2015). Red squares and circles are high-z AGNs (z > 4; Y. Harikane et al. 2023; R. Maiolino et al. 2024, respectively). The MBH–M⋆ relations from J. E. Greene et al. (2020) for all galaxies and late-type only are shown in black (±0.81 dex scatter around the mean) and blue (±0.65 dex), respectively. The ωCen/GSE, where ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })=8.5﹩ is plotted as the green star symbol (T. M. Callingham et al. 2022). The green ±0.3 dex stripe covers the typical M⋆ reported in literature for GSE (see text). The IMBH mass range allowed by the M. Häberle et al. (2024) analysis is displayed as the green dotted lines. Other IMBH detections, namely NGC 205 (orange diamond with black edge; D. D. Nguyen et al. 2019) and NGC 4395 (blue pentagon; J.-H. Woo et al. 2019), are also plotted. The ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })=7.5﹩ of Sagittarius dSph is represented by the purple dashed line (T. M. Callingham et al. 2022). M31 stellar clusters with candidate IMBHs are the blue hexagons with black edges (K. Gebhardt et al. 2002; R. Pechetti et al. 2022). For these M31 candidates, I adopt cluster masses as lower limits to their host M⋆. Black dotted lines represent different values for the MBH/M⋆ ratio.
Paper: Black Hole Scaling Relations in the Dwarf-galaxy Regime with Gaia-Sausage/Enceladus and ωCentauri
Authors: Guilherme Limberg
Figure caption: MBH–σ⋆. Symbols and colors follow the scheme of Figure 1; blue and orange diamonds are late- and early-type galaxies, respectively (J. E. Greene et al. 2020), triangles are constraining MBH upper limits (also J. E. Greene et al. 2020), MW in yellow (R. Genzel et al. 2010), M31 stellar clusters with candidate IMBHs as the blue hexagons (K. Gebhardt et al. 2002; R. Pechetti et al. 2022), and ωCen (GSE) in dark green (σ⋆ from R. Pechetti et al. 2024). Blue squares are UCDs with massive BHs detected (see text). Pink pentagons are dwarf AGNs with σ⋆ measurements from V. F. Baldassare et al. (2020). Other IMBH detections, NGC 205 (orange diamond with black edge; D. D. Nguyen et al. 2019) and NGC 4395 (blue pentagon; J.-H. Woo et al. 2019), are also shown. The σ⋆ value of NGC 6715/M54 is the purple dashed line (M. Alfaro-Cuello et al. 2020). The MBH–σ⋆ relations from J. E. Greene et al. (2020) are plotted in black (±0.55 dex scatter) and blue (±0.58 dex) for all galaxies and late-type only, respectively.
Paper: Black Hole Scaling Relations in the Dwarf-galaxy Regime with Gaia-Sausage/Enceladus and ωCentauri
Authors: Guilherme Limberg
Figure caption: MBH–redshift. The corresponding time since Big Bang is calculated with Planck Collaboration et al. (2020) cosmology (upper axis). Symbols and colors follow the same scheme of Figure 1: red squares and circles for high-z AGNs (Y. Harikane et al. 2023; R. Maiolino et al. 2024, respectively), Milky Way in yellow (R. Genzel et al. 2010), and ωCen/GSE in dark green. Purple line represents a previous, perhaps first, pericenter of Sagittarius dSph (T. Ruiz-Lara et al. 2020). BH growth tracks calculated as in X. Fan et al. (2023, see text) are shown as the orange (heavy seed) and gray (light seed) lines. The range of initial masses are 10–100 M⊙ ​​​​​​ for light seeds and 5000–20,000 M⊙ for heavy ones.
Paper: Black Hole Scaling Relations in the Dwarf-galaxy Regime with Gaia-Sausage/Enceladus and ωCentauri
Authors: Guilherme Limberg
Figure caption: MNSC–M⋆. Blue and orange diamonds represent late- and early-type galaxies, respectively. The MNSC–M⋆ relation is the black line (±0.6 dex scatter as the shaded region; N. Neumayer et al. 2020). Squares are different MW candidate NSCs and host galaxies (see text): M54/Sagittarius (purple), NGC 6273/Kraken (red), and NGC 6934/Helmi streams (blue). ωCen/GSE is in green. Black dotted lines represent different values for the MNSC/M⋆ ratio.
Paper: Two Novel Hot Jupiter Formation Pathways: How White Dwarf Kicks Shape the Hot Jupiter Population
Authors: Alexander P. Stephan, David V. Martin, Smadar Naoz, Nathan R. Hughes, Cheyanne Shariat
Figure caption: Evolution of a binary star system that forms an HJ after both stars have become white dwarfs. The line colors used in this plot correspond to the same parameters as shown in Figures 2 and 3, with the addition of magenta for the primary star’s Roche limit. In this system, the EKL oscillations are initially not very significant and do not increase in strength after the first WD kick (left column of panels). However, the second WD formation kick (middle column of panels) is able to alter the companion inclination, SMA, and eccentricity sufficiently to trigger stronger EKL evolution, which eventually leads to HJ formation (right column of panels). The planet host star has an initial mass of m1 = 1.235 M⊙; the planet has the mass and radius of Jupiter, an initial orbit SMA of a1 = 8.265 au, and eccentricity of e1 = 0.01; and the stellar companion has an initial mass of m3 = 1.986 M⊙, initial orbit SMA of a2 = 251.948 au, and eccentricity of e2 = 0.412. The planetary and stellar orbits have an initial mutual inclination of inc =53﹩\mathop{.}\limits^{\circ }﹩358 and arguments of periapsis of ω1 = 90﹩\mathop{.}\limits^{\circ }﹩174 and ω2 = 7﹩\mathop{.}\limits^{\circ }﹩237, respectively.
Paper: Two Novel Hot Jupiter Formation Pathways: How White Dwarf Kicks Shape the Hot Jupiter Population
Authors: Alexander P. Stephan, David V. Martin, Smadar Naoz, Nathan R. Hughes, Cheyanne Shariat
Figure caption: Likelihood of binary disruption vs. prekick stellar binary period for HJ-forming systems in our simulations. Shown is the likelihood that a particular HJ-forming system in our simulations is disrupted by the WD formation kick vs. the orbital period of the stellar binary, P2, just before WD formation, color coded by the mass of the stellar binary. The cyan, blue, and magenta lines show the disruption likelihood vs. orbital period for stellar binaries with eccentricity 0.6 and with total masses of 0.7, 1.2, and 2.5 M⊙, respectively. Note that these are the masses toward the end of the AGB, when some significant mass loss has already occurred. Overall, our sample of HJ systems will undergo binary disruption from the WD formation kick in about 50% of cases, about 55% when considering the orbital stability of the postkick system.
Paper: Protosolar D-to-H Abundance and One Part per Billion PH3 in the Coldest Brown Dwarf
Authors: Melanie J. Rowland, Caroline V. Morley, Brittany E. Miles, Genaro Suarez, Jacqueline K. Faherty, Andrew J. Skemer, Samuel A. Beiler, Michael R. Line, Gordon L. Bjoraker, Jonathan J. Fortney, Johanna M. Vos, Sherelyn Alejandro Merchan, Mark Marley, Ben Burningham, Richard Freedman, Ehsan Gharib-Nezhad, Natasha Batalha, Roxana Lupu, Channon Visscher, Adam C. Schneider, T. R. Geballe, Aarynn Carter, Katelyn Allers, James Mang, Dániel Apai, Mary Anne Limbach, Mikayla J. Wilson
Figure caption: The corner plot of a subset of retrieved parameters from the GTO spectrum (pink) and the time-averaged GO spectrum (blue). The discrepancy between the retrieved radial velocities is believed to be due to differences in wavelength calibration in the two pipelines. An upper limit for the cloud VMR is shown, and other cloud parameters were unconstrained. Top panel: the CCF computed for the GO data set with the CH3D model (top) or PH3 model (bottom) and residuals (observed spectrum minus the best-fit model with the relevant opacity removed). The CCF is normalized by the standard deviation outside of the CCF peak so that the y-axes of the right-hand panels represent the S/N of the CCF peak.
Paper: Protosolar D-to-H Abundance and One Part per Billion PH3 in the Coldest Brown Dwarf
Authors: Melanie J. Rowland, Caroline V. Morley, Brittany E. Miles, Genaro Suarez, Jacqueline K. Faherty, Andrew J. Skemer, Samuel A. Beiler, Michael R. Line, Gordon L. Bjoraker, Jonathan J. Fortney, Johanna M. Vos, Sherelyn Alejandro Merchan, Mark Marley, Ben Burningham, Richard Freedman, Ehsan Gharib-Nezhad, Natasha Batalha, Roxana Lupu, Channon Visscher, Adam C. Schneider, T. R. Geballe, Aarynn Carter, Katelyn Allers, James Mang, Dániel Apai, Mary Anne Limbach, Mikayla J. Wilson
Figure caption: The PH3 abundance as a function of Teff for Y dwarfs with detections or upper limits from S. A. Beiler et al. (2024a), A. J. Burgasser et al. (2024), J. K. Faherty et al. (2024), C. E. Hood et al. (2024), H. Kothari et al. (2024), and this work, along with the global PH3 abundance of Jupiter from L. N. Fletcher et al. (2009). The * indicates recalculated upper limits from S. A. Beiler et al. (2024a). The gray and black lines show the Elf Owl PH3 abundance at 3 bars for various mixing strengths and effective temperatures. All models assume log(g) = 4, cloud-free, solar metallicity, and solar C/O atmospheres. Models extend down to 275 K. WISE 0855 is consistent with very slow (log(Kzz) < 2 cm2 s−1) mixing.
Paper: Protosolar D-to-H Abundance and One Part per Billion PH3 in the Coldest Brown Dwarf
Authors: Melanie J. Rowland, Caroline V. Morley, Brittany E. Miles, Genaro Suarez, Jacqueline K. Faherty, Andrew J. Skemer, Samuel A. Beiler, Michael R. Line, Gordon L. Bjoraker, Jonathan J. Fortney, Johanna M. Vos, Sherelyn Alejandro Merchan, Mark Marley, Ben Burningham, Richard Freedman, Ehsan Gharib-Nezhad, Natasha Batalha, Roxana Lupu, Channon Visscher, Adam C. Schneider, T. R. Geballe, Aarynn Carter, Katelyn Allers, James Mang, Dániel Apai, Mary Anne Limbach, Mikayla J. Wilson
Figure caption: Comparison of reduced spectra within the region most impacted by CH3D absorption. Top panel: the GTO spectrum (blue) plotted with the GO spectrum (pink). The GO spectrum is interpolated onto the same wavelength grid as the GTO spectrum. Bottom panel: the ratio of the GTO spectrum divided by the GO spectrum (black dots). The yellow dashed line is a reference for no difference. The top of the pink area is the ratio of the brightest spectrum divided by the dimmest spectrum in the time series. The bottom of the pink area is the dimmest spectrum divided by the brightest spectrum.
Paper: Protosolar D-to-H Abundance and One Part per Billion PH3 in the Coldest Brown Dwarf
Authors: Melanie J. Rowland, Caroline V. Morley, Brittany E. Miles, Genaro Suarez, Jacqueline K. Faherty, Andrew J. Skemer, Samuel A. Beiler, Michael R. Line, Gordon L. Bjoraker, Jonathan J. Fortney, Johanna M. Vos, Sherelyn Alejandro Merchan, Mark Marley, Ben Burningham, Richard Freedman, Ehsan Gharib-Nezhad, Natasha Batalha, Roxana Lupu, Channon Visscher, Adam C. Schneider, T. R. Geballe, Aarynn Carter, Katelyn Allers, James Mang, Dániel Apai, Mary Anne Limbach, Mikayla J. Wilson
Figure caption: Left panel: the retrieved posteriors for the gas-phase abundances and log(g) for the GTO spectrum (pink) and GO spectrum (blue). All gases are constrained with the exception of 13CO. Right panel: the retrieved log(﹩\tfrac{{\mathrm{CH}}_{3}{\rm{D}}}{{\mathrm{CH}}_{4}}﹩)E posterior from the GO spectrum (blue) and a simulated spectrum based on the best-fit model with CH3D opacity set to 0. The bounded constraint from the actual data and the upper limit from the synthetic data indicate that CH3D information exists in NIRSpec/G395M data.
Paper: Protosolar D-to-H Abundance and One Part per Billion PH3 in the Coldest Brown Dwarf
Authors: Melanie J. Rowland, Caroline V. Morley, Brittany E. Miles, Genaro Suarez, Jacqueline K. Faherty, Andrew J. Skemer, Samuel A. Beiler, Michael R. Line, Gordon L. Bjoraker, Jonathan J. Fortney, Johanna M. Vos, Sherelyn Alejandro Merchan, Mark Marley, Ben Burningham, Richard Freedman, Ehsan Gharib-Nezhad, Natasha Batalha, Roxana Lupu, Channon Visscher, Adam C. Schneider, T. R. Geballe, Aarynn Carter, Katelyn Allers, James Mang, Dániel Apai, Mary Anne Limbach, Mikayla J. Wilson
Figure caption: D/H ratio as a function of object mass as measured in the ISM (gray), terrestrial planets, ice giants, gas giants (M. J. Drake 2005; P. Hartogh et al. 2011; L. I. Cleeves et al. 2014), and brown dwarfs as predicted from D. S. Spiegel et al. (2011; dark gray line), with the retrieved D/H measurement of WISE 0855 in black. The mass estimate is derived from the retrieved log(g) with a radius of 1.0 RJup.
Paper: Protosolar D-to-H Abundance and One Part per Billion PH3 in the Coldest Brown Dwarf
Authors: Melanie J. Rowland, Caroline V. Morley, Brittany E. Miles, Genaro Suarez, Jacqueline K. Faherty, Andrew J. Skemer, Samuel A. Beiler, Michael R. Line, Gordon L. Bjoraker, Jonathan J. Fortney, Johanna M. Vos, Sherelyn Alejandro Merchan, Mark Marley, Ben Burningham, Richard Freedman, Ehsan Gharib-Nezhad, Natasha Batalha, Roxana Lupu, Channon Visscher, Adam C. Schneider, T. R. Geballe, Aarynn Carter, Katelyn Allers, James Mang, Dániel Apai, Mary Anne Limbach, Mikayla J. Wilson
Figure caption: The corner plot of derived parameters and the P(T) profile of the fiducial retrieval on the GTO spectrum (pink) and the time-averaged GO spectrum (blue). The dashed lines in the P(T) plot show the normalized flux-averaged contribution for each layer in the atmosphere, and the opaqueness of the P(T) profile corresponds to this value, with a minimum of 20% for visibility.
Paper: Volatile-rich Sub-Neptunes as Hydrothermal Worlds: The Case of K2-18 b
Authors: Cindy N. Luu, Xinting Yu, 馨婷 余, Christopher R. Glein, Hamish Innes, Artyom Aguichine, Joshua Krissansen-Totton, Julianne I. Moses, Shang-Min Tsai, Xi Zhang, Ngoc Truong, Jonathan J. Fortney
Figure caption: (a) Phase diagram of pure water, showing adiabats for six selected ocean temperatures from 647.15 K to 1273.15 K at a pressure of redox equilibrium of 1 kbar as an example. This plot is most relevant to cases with lower H2 abundances in the fluid envelope. Liquid water will be saturated at lower temperatures for the highest H2 abundance considered in this work (see Appendix G). (b) A schematic diagram showing the upper interior structure of K2-18 b with a miscible supercritical H2+H2O layer (B. Benneke et al. 2024) or (c) with phase-separated H2-rich and H2O-rich layers and a cloud layer in an H2–He-dominated atmosphere. Star and circle symbols represent where aqueous and gaseous calculations are performed, respectively.
Paper: Volatile-rich Sub-Neptunes as Hydrothermal Worlds: The Case of K2-18 b
Authors: Cindy N. Luu, Xinting Yu, 馨婷 余, Christopher R. Glein, Hamish Innes, Artyom Aguichine, Joshua Krissansen-Totton, Julianne I. Moses, Shang-Min Tsai, Xi Zhang, Ngoc Truong, Jonathan J. Fortney
Figure caption: Panels (a)–(c) and panels (d)–(f) show the calculated aqueous and gaseous CH4/CO2 ratios at ﹩{X}_{{\rm{H}\,}_{2}\,\rm{O}}﹩ = 99.6%, 90.0%, and 42.4%. The ﹩{X}_{{\rm{H}\,}_{2}\,\rm{O}}﹩ = 42.4% results are in dashed lines to imply that the results are illustrative, as this concentration describes a hydrogen-rich fluid (see Appendix D). The black dashed line and gray region represent the CH4/CO2 ratio and uncertainty presented in N. Madhusudhan et al. (2023b).