adsabs/AstroCLIMB huggingface dataset:
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Left: the SED-derived SFR vs. the stellar mass for galaxies in the NGDEEP final sample (dots) and low-SNR sample (triangle) color-coded by their redshift. The median SFR and stellar mass for galaxies in the final sample at z ∼ 2 and z ∼ 3 are shown (in both panels) in black purple- and orange-filled dots, respectively. For comparison, the SFMS for galaxies at 2.0 < z < 2.5 from K. E. Whitaker et al. (2014) is shown down to their mass completeness in the pink line and extended to the lower stellar mass region in the dashed line. Right: the median SFR and stellar mass are shown for galaxies at various redshifts: z ∼ 1.7 from CLEAR (C. Papovich et al. 2022, open blue squares), z ∼ 2.3 and z ∼ 3.3 from the MOSDEF stacked sample (R. L. Sanders et al. 2021, open magenta and orange diamonds), z ∼ 0 from SDSS (brown crosses), z ∼ 0 from CLASSY (D. A. Berg et al. 2022, filled cyan triangles), green pea galaxies at z ∼ 0 (H. Yang et al. 2017b, filled green triangles) and blueberry galaxies at z ∼ 0 (H. Yang et al. 2017a, filled blue triangles). The SDSS sample is shown in the 2D histograms in black. The same median values from the NGDEEP final sample as left are shown in black purple- and orange-filled dots. The NGDEEP O32 sample has consistently higher SFR than the SFMS at z ∼ 2–2.5, and has a similar SFR with those of extreme galaxies at z ∼ 0.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Left: the O32 ratio vs. stellar mass for galaxies in the NGDEEP final sample (dots) and low-SNR sample (triangle), color-coded by redshift. The median O32 along the abscissa is shown for galaxies in the final sample (open black circles), for those at z ∼ 2 and z ∼ 3 in purple- and orange-filled dots, respectively. The best fit for the NGDEEP final sample with stellar mass >108.5 M ⊙ is shown as the solid black lines, and extended to lower stellar mass as the dashed line. The gray region marks the 1σ total scatter. Right: the median O32 ratios as a function of SFR are shown for CLEAR, MOSDEF, SDSS, CLASSY, green peas, and blueberry galaxies (symbols are the same as in Figure 3). The SDSS sample is shown in the 2D histograms in black. The same median values and fits from the NGDEEP final sample are shown, identical to those in the left panel. The NGDEEP sample shows a tight mass–O32 relation.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Left: the O32 vs. SFR for galaxies in the NGDEEP final sample (dots) and low-SNR sample (triangle), color-coded by redshift. The median O32 values along the abscissa are shown for galaxies at z ∼ 2 and z ∼ 3 in purple- and orange-filled dots, respectively. The best fit for galaxies with stellar mass >108.5 M ⊙ at z ∼ 2 and z ∼ 3 are shown as the solid purple and orange lines, and extended to lower SFR as the dashed line. The color-shaded region marks the 1σ total scatter for each redshift sample. Right: the median O32 ratios as a function of SFR are shown for CLEAR, MOSDEF, SDSS, CLASSY, green peas, and blueberry galaxies (symbols are the same as in Figure 3). The SDSS sample is shown in the 2D histograms in black. The same median values and fits from the NGDEEP O32 sample are shown, identical to those in the left panel. The NGDEEP sample shows a negative SFR–O32 relation, with a dependence on redshift.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Left: the stellar mass histograms for NGDEEP full sample (blue), final sample (red), and “photometric” galaxies (black). The latter includes all galaxies with photometry redshift (spectroscopic redshift if available) at 1.7 < z < 3.4 (gray). The histogram for the photometric galaxies is rescaled to match the massive end of that for NGDEEP galaxies. Middle: the PDF of stellar mass for NGDEEP final sample (red), and the final sample separated by redshift with 1.7 < z < 2.5 and 2.5 < z < 3.4 (purple and orange, respectively). The fitted skew-normal distribution for the NGDEEP final sample is shown in a black dashed line. In both panels, the vertical dashed line marks the mass completeness of 108.50 M ⊙. Right: the redshift histograms of the final sample at 1.7 < z < 2.5 and 2.5 < z < 3.4 (purple and orange, respectively). Colored vertical lines indicate the median redshifts.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Left: the O32 vs. sSFR for galaxies in the NGDEEP final sample (dots) and low-SNR sample (triangles), color-coded by stellar mass. The median O32 values along the abscissa are shown for galaxies at z ∼ 2 and z ∼ 3 in purple- and orange-filled dots, respectively. The best fit for galaxies with stellar mass >108.5 M ⊙ is shown as the solid black lines, and extended to lower/higher sSFR as the dashed line. The gray region marks the 1σ total scatter. Left: the median O32 ratios as a function of sSFR are shown for CLEAR, MOSDEF, SDSS, CLASSY, green peas, and blueberry galaxies (symbols are the same as in Figure 3). The SDSS sample is shown in the 2D histograms in black. The same median values and fits from the NGDEEP final sample are shown, identical to those in the left panel. Note that the x-axis scale of the right panel is more extended. NGDEEP galaxies show a positive sSFR–O32 relation without a redshift dependence between z ∼ 1.7 and 3.4, but with a large scatter.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: SNR of emission lines as a function of emission line flux for NGDEEP galaxies at 1.7 < z < 3.4. Emission lines include [O II]λλ3726,3729, Hβ, [O III]λλ4959,5007, and Hα across three filters (F115W, F150W, and F200W).
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: TDE rate Γ for each galaxy or cluster in our sample. Three different populations of MBHs are shown, denoted with different colors: all IMBH-GNs in red, all IMBH-GCs in blue, and all SMBHs in green. Panel (a) shows Γ plotted against MBH. We adopt MBH,best (filled symbols) for an MBH if a best mass measurement exists; otherwise, we use ﹩{M}_{{\rm{BH}},{\rm{\max }}}﹩ (open symbols) if only a maximum mass measurement exists. Panel (b) is the same as panel (a) but includes additional histograms (blue shaded regions) showing the averaged TDE rate distribution and a broken power-law fit (blue line) for the averaged Γ–MBH relation (Equation (18)). One can see that Γ increases with MBH in the IMBH regime but decreases with MBH in the SMBH regime. Panel (c) shows Γ plotted against the total stellar mass of a galaxy or cluster M⋆. Panel (d) shows Γ plotted against the mass of the innermost stellar component when a galaxy can be fitted with multiple components. Galaxies with an NSC as the innermost component are represented using star symbols instead of circles.
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: MBH mass MBH, individual galaxy TDE rate Γ, and TDE pinhole fraction f (from top to bottom) plotted against the Sérsic inner slope p, central density ρ0, and effective radius Reff (from left to right) for our IMBH and SMBH samples. The symbol style and colors are consistent with Figure 1(d), except in panels (g), (h), and (i), where the SMBHs are further divided into two subgroups: MBH > 107 M⊙ (turquoise) and 106 M⊙ < MBH < 107 M⊙ (orange). In panels (d) and (e), the red and green lines also display the fitting functions (Equations (22) and (23)) for IMBH-GN hosts and SMBH hosts, respectively.
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: The BHMFs and the volumetric TDE rate. Panel (a) shows the BHMF from E. Gallo & A. Sesana (2019) in blue and that from H. Cho & J.-H. Woo (2024) (after the correction with the AGN duty cycle and type 1 fraction) in orange. Panel (b) shows the volumetric TDE rate ﹩\dot{N}﹩ vs. MBH. The histograms are obtained from convolving the binned average of the IMBH-GN and SMBH TDE rates (similar to the histogram shown in Figure 1(b)) with the BHMFs shown in panel (a). The blue line shows the fitting function (Equation (28)) for the volumetric rate computed using the BHMF from E. Gallo & A. Sesana (2019). Comparison to observations is also shown using dashed lines: D. Lin et al. (2018) and C. R. Angus et al. (2022) reported volumetric IMBH TDE rates of ∼10−8 Mpc−3 yr−1 based on the observation of J2150-055 and AT 2020neh, respectively, and Y. Yao et al. (2023) reported the volumetric TDE rate as a function of MBH based on the 33 optically selected ZTF TDEs.
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: The stellar density profiles of galaxies and clusters hosting IMBH-GNs (left panel) and IMBH-ONs (right panel). The shaded region shows the 1σ range of the stellar density profiles of the galaxies hosting SMBHs for comparison.
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: The difference between the observed BH mass MBH,obs and the BH mass at which Γ(MBH) reaches maximum MBH,peak, plotted against MBH,obs, for each galaxy or cluster in our sample. The color indicates the difference in TDE rates calculated at MBH,peak and MBH,obs. A linear fit is shown using the solid blue line. The dashed blue lines indicate where the y-axis is 0 (i.e., where ﹩{\rm{\Delta }}\mathrm{log}\,{M}_{{\rm{BH}}}﹩ switches sign), which crosses the linear fit at ﹩\mathrm{log}\,{M}_{{\rm{BH,obs}}}\sim 7﹩.
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: TDE rate Γ from each galaxy or cluster as a function of MBH (while keeping the stellar profiles fixed) from IMBHs (top panel) and SMBHs (bottom panel). Solid lines and dotted lines in the top panel represent IMBH-GNs and IMBH-ONs, respectively. The circles mark the observed BH masses MBH,obs and the corresponding TDE rates.
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: Pinhole fraction f plotted against MBH and M⋆. The symbols and colors are the same as in Figure 1. The orange curves represent the fitting functions (Equations (20) and (21)).
Paper: Rates of Stellar Tidal Disruption Events around Intermediate-mass Black Holes
Authors: Janet N. Y. Chang, Lixin Dai, Hugo Pfister, Rudrani Kar Chowdhury, Priyamvada Natarajan
Figure caption: The distribution of penetration parameter β in TDEs for different MBH. The curves are color-coded by MBH, from 108 M⊙ (green) to 104 M⊙ (red). The dashed line denotes the dP/dβ ∝ β−2 relation that characterizes the pinhole-dominated regime.
Paper: TRAPPIST-1 d: Exo-Venus, Exo-Earth, or Exo-Dead?
Authors: M. J. Way
Figure caption: Surface temperature (straddling 0°C), total cloud cover (%), net outgoing thermal radiation (W m−2), and cloud water content (kg m−2) for four of the simulations listed in Table 1. Simulations are displayed from dry (Sim 01: Arid-Venus), semidry 10 m GEL (Sim 02: 10 m-Venus), Earth-like 310 m GEL (Sim 03: 310 m-Venus), and an aquaplanet (Sim 06). Sims 01–03 are 1 bar N2 dominated with 400 ppmv CO2. Sim 06 is N2 dominated, but the only greenhouse gas is H2O following E. T. Wolf (2017). Cloud coverage is fairly low in Sims 01–02, as expected given limited surface reservoirs and cloud water content (rightmost column), and is much higher for Sims 03 and 06.
Paper: TRAPPIST-1 d: Exo-Venus, Exo-Earth, or Exo-Dead?
Authors: M. J. Way
Figure caption: TRAPPIST-1 d temperature and specific humidity as a function of model pressure layers. Top row: 1000 mb; bottom row: 500 mb. The vertical dotted black line in the right panels represents the moist greenhouse limit of 3  ×  10−3 (v v−1) from J. F. Kasting et al. (1993). We include a modern Earth simulation as a comparison, but note that it uses 20 vertical layers, whereas all other simulations use 40.
Paper: TRAPPIST-1 d: Exo-Venus, Exo-Earth, or Exo-Dead?
Authors: M. J. Way
Figure caption: This is (a) the NRB at the TOA and (b) the mean global surface temperature for the last 240 orbits of each simulation. The legend is the same as that used in Figure 1. The large fluctuations seen in the magenta line with large circles (Sim 09 AP W2) correspond with the large imbalance seen in Table 1 for this experiment.
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Sensitivity model results using high concentrations of total ammonia in the high H2 case (here, low N is 0.01 mole NH3+NH4+/kg H2O; high N is 0.1 mole NH3+NH4+/kg H2O; L. M. Fifer et al. 2022). The gray shaded area represents the preferred pH range (pH ≈ 8–9) of L. M. Fifer et al. (2022). See Table A3 for other model settings.
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Simulated concentrations of dissolved Fe and S under various boundary conditions of Enceladus’s ocean (see Table A3 for detailed settings of (a)–(d) at 0°C). [C] denotes the total concentration of carbonate ions: HCO3− + CO32−, and H2/CO2 indicates the molar concentration ratio of dissolved H2 and CO2 (see Table A3).
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Effect of suppressing pyrite precipitation on simulated dissolved sulfur concentrations in the Enceladus ocean. The nominal model results allowing pyrite precipitation are shown in gray for comparison. The upper limit on dissolved sulfur (black dashed line; based on observations of the Cassini) is from B. Magee & J. Waite (2017) and C. Ray et al. (2021). [C] denotes the total concentration of carbonate ions: HCO3− + CO32−, and H2/CO2 indicates the molar concentration ratio of dissolved H2 and CO2 (see Table A3).
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Effect of dissolved silica on simulated concentrations of Fe and S under various boundary conditions of Enceladus’s ocean (see Table A3 for detailed settings of (a)–(d) at 0°C). Different concentrations of silica are achieved by assuming the solubility equilibrium with common SiO2 minerals. [C] denotes the total concentration of carbonate ions: HCO3− + CO32−, and [H2] case indicates the molar concentration ratio of dissolved H2 and CO2 (see Table A3). Note the different vertical scales of the top and bottom plots.
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Proportions of dissolved Fe from our model at 0°C and various pH values. These species account for 99% or more of the dissolved Fe inventory. [C] denotes the total concentration of carbonate ions: HCO3− + CO32−, and [H2] case indicates the molar concentration ratio of dissolved H2 and CO2 (see Table A3).
Paper: A Study on the Line of Sight to Galaxies Detected at Gamma-Ray Energies
Authors: Amy Furniss, Josepf N. Amador, Olivier Hervet, Ollie Jackson, David A. Williams
Figure caption: Top panels: the voidiness distributions of the 4LAC AGN (blue line), shown along with the contours one and two standard deviations from the median of the randomized populations (blue shaded regions), calculated in each voidiness bin in the nearby (left) and distant (right) redshift intervals, respectively. The 4LAC AGN data are available as the data behind the figure. Bottom panels: the CDF for the observed 4LAC voidiness (blue line) and the one and two sigma contours from the median of the randomized populations, calculated in each displayed voidiness bin. In all panels the redshift-matched SDSS QSO populations’ one and two standard deviation contours are shown in red shading. The data, which include the source name, location, redshift, and calculated voidness, are available in the online journal as a data behind the figure (dbF) file.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Study on the Line of Sight to Galaxies Detected at Gamma-Ray Energies
Authors: Amy Furniss, Josepf N. Amador, Olivier Hervet, Ollie Jackson, David A. Williams
Figure caption: Top panels: the voidiness distributions of the observed SDSS QSOs (black line), shown along with the contours for one and two standard deviations from the median of the randomized populations (gray shaded regions), calculated per displayed voidiness bin in the nearby (left) and distant (right) redshift intervals, respectively. The SDSS QSO data are available as the data behind the figure. Bottom panels: the CDFs for the observed SDSS QSOs (black line) and contours one and two sigma from the median of the randomized populations in the nearby (left) and distant (right) redshift intervals. The data, which include the source name, location, redshift, and calculated voidness, are available in the online journal as a data behind the figure (dbF) file.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Study on the Line of Sight to Galaxies Detected at Gamma-Ray Energies
Authors: Amy Furniss, Josepf N. Amador, Olivier Hervet, Ollie Jackson, David A. Williams
Figure caption: The redshift distributions of the SDSS QSOs (blue dashed line) and 4LAC AGN (orange line) within the footprint of the P. M. Sutter et al. (2012, 2014) void catalogs. A redshift-matched SDSS QSO population (dotted green) is also shown.
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Predicted concentrations of dissolved Fe and S in Enceladus ocean water compared to serpentinization fluids on Earth. The symbols in (a) and (c) show different model boundary settings for the concentrations of total carbonate species and the H2,aq/CO2,aq ratio (Table A3). The dark gray shaded area shows the predicted concentrations of dissolved Fe in (a) and (b), and those of dissolved S in (c) and (d). The observationally based upper limit on dissolved sulfur (black dashed line) in (c) and (d) is from B. Magee & J. Waite (2017) and C. Ray et al. (2021). The concentrations of dissolved Fe and S in serpentinization fluids on Earth (filled circles in (b) and (d)) were compiled from the literature (P. L. Morrill et al. 2013; W. E. Seyfried et al. 2015; K. R. Rempfert et al. 2017; E. M. Fones et al. 2019; E. A. Kraus et al. 2021; J. A. M. Leong et al. 2021; K. A. Aquino et al. 2022; L. R. Trutschel et al. 2022). One should note that the S concentration of Lost City fluids was concluded to be seriously contaminated by terrestrial seawater (W. E. Seyfried et al. 2015; K. A. Aquino et al. 2022), so only their HS− concentrations are plotted (in red triangles). The inferred pH range of Enceladus ocean water (light gray shaded area) comes from C. R. Glein et al. (2018), and the dissolved levels of Fe and S in modern Earth seawater (olive green box and line) are from E. K. Berner & R. A. Berner (2012).
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Simulated equilibrium mineralogy on the ocean floor under various nominal conditions of Enceladus’s ocean (see Table A3 for detailed settings) at 0°C. [C] denotes the total concentration of carbonate ions: HCO3− + CO32−, and [H2] case indicates the molar concentration ratio of dissolved H2 and CO2 (see Table A3).