adsabs/AstroCLIMB huggingface dataset:
Paper: Observability of Isolated Stellar-mass Black Holes
Authors: Lena Murchikova, Kailash C. Sahu
Figure caption: Estimated emission spectra of an IsoBH with different masses and velocities located 200 pc from the Sun, accreting from the ISM with a density of 100 cm−3. We show how the spectra change with IsoBH mass: 3 M⊙ (dashed gray line), 10 M⊙ (dashed gray-cyan line), and 30 M⊙ (gray line), all moving at 50 km s−1. We also show the effect of varying velocity for a 10 M⊙: 10 km s−1 (dashed cyan line), 50 km s−1 (dashed gray-cyan line), and 200 km s−1 (cyan line). In each case, the solid line corresponds to the highest value of the parameter being varied. The IsoBH is assumed to accrete at 1% of the Bondi rate (λ = 0.01). For convenience, the spectra are presented in two different units (νFν and Fν) commonly used in different wavelength regions.
Paper: Contemporaneous X-Ray and Optical Polarization of Extremely High-synchrotron-peaked Blazar H 1426+428
Authors: Anuvab Banerjee, Akash Garg, Divya Rawat, Svetlana Jorstad, Alan P. Marscher, Ivan Agudo, Jorge Otero-Santos, Daniel Morcuende, Juan Escudero Pedrosa, Alberto Domínguez, Ayan Bhattacharjee, Isaiah Cox, Indrani Pal, Xiurui Zhao, Andrealuna Pizzetti, Stefano Marchesi, Núria Torres-Albà, Kouser Imam, Ross Silver, Marco Ajello
Figure caption: Top-left panel shows the XSPEC fit of Swift-XRT spectra using a power-law model corresponding to the observation on 2024 May 27. The top-middle and top-right panels show the simultaneous fit of Stokes Q and U spectra, respectively, including all DUs. Bottom panels show the corresponding fit residuals.
Paper: Generation of Magnetic Fields around Black Hole Accretion Disks due to Nonconservative Radiation Fields
Authors: Mukesh Kumar Vyas, Asaf Pe'er
Figure caption: Same as Figure 2, but with the addition of a corona having luminosity lc = 1. Note the orders-of-magnitude difference in the magnitude of the magnetic field components relative to the results in Figure 2.
Paper: Generation of Magnetic Fields around Black Hole Accretion Disks due to Nonconservative Radiation Fields
Authors: Mukesh Kumar Vyas, Asaf Pe'er
Figure caption: The three components of the magnetic field contours in the r–z plane for an accretion disk truncating at 3 Schwarzschild radii (rg) when a corona component is absent. The mass of the BH is 10 M⊙, and the accretion rate considered is 1 Eddington accretion rate.
Paper: Generation of Magnetic Fields around Black Hole Accretion Disks due to Nonconservative Radiation Fields
Authors: Mukesh Kumar Vyas, Asaf Pe'er
Figure caption: Top: dependence of the maximum magnetic field produced above the disk (﹩{B}_{{\rm{\max }}}﹩) on the corona size (rs), with other parameters the same as considered in Section 4.2. Bottom: dependence of the maximum field strength (G) with corona luminosity lc given in Eddington units, for fixed corona size, rs = 3rg.
Paper: Generation of Magnetic Fields around Black Hole Accretion Disks due to Nonconservative Radiation Fields
Authors: Mukesh Kumar Vyas, Asaf Pe'er
Figure caption: Geometry of the accretion disk with two distinct components, an outer Keplerian disk and an inner radiating corona separated at distance rd = rs.
Paper: Generation of Magnetic Fields around Black Hole Accretion Disks due to Nonconservative Radiation Fields
Authors: Mukesh Kumar Vyas, Asaf Pe'er
Figure caption: Structure of the resultant magnetic field in the vicinity of the accretion disk corresponding to parameters in Figure 3.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: The WFe II/WMg II ratio plotted against ﹩{\mathrm{log}}\,(1+z)﹩ (left) and the D (right). Different colors represent various Fe II lines, as indicated in the legend, with markers added in the left panel to show the corresponding impact parameter bins. The gray lines depict linear fits along with their uncertainties. We also fit data in different impact parameter bins separately, with slopes and uncertainties labeled in corresponding colors. The data clearly show that the WFe II/WMg II ratio decreases with increasing redshift z.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: Top panel: an example of the spectrum of the background quasar and its QSOFit, with the region below 1230 Å magnified. Bottom panel: the fraction of flux at different wavelengths contributed by the background Lyα forest region. The marker and color represent the element and the absorption line wavelength, respectively, as in Figure 2 . The x-axis represents measurements of W that include flux points within the Lyα absorption forest, while the y-axis represents measurements with those points excluded.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: Equivalent width Wi for various absorption lines of Fe II (left panel) and Ni II (right panel). The x-axis represents different absorption lines for each ion, and the color of the data points indicates the redshift z, with the color bar on top showing the corresponding redshift range.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: Similar to Figure 2, this plot includes data for ELGs, LRGs, and QSOs. Filled colored markers represent ELGs, open colored markers represent LRGs, and open black markers represent QSOs.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: Carbon disequilibrium chemistry and water clouds are likely in 14 Her c’s atmosphere. JWST/NIRCam photometry of 14 Her c (F444W flux as a black hexagon, F200W upper limit as a black triangle) compared to atmospheric model spectra (colored lines) integrated over the filter bandpasses (colored circles, squares, and diamonds). Publicly available Sonora Bobcat (M. S. Marley et al. 2021) and Sonora Elf Owl (S. Mukherjee et al. 2024) models (in dark blue and green, respectively) are unable to reproduce the data with temperatures in agreement with evolutionary model predictions. Custom PICASO models with an updated treatment of carbon disequilibrium chemistry (light blue) bring the models into better alignment with the observations and evolutionary model predictions. Adding water-ice clouds (red) to these custom atmospheric models brings the observations into agreement at 1σ with both the atmospheric and evolutionary models.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: The stellar RVs driven by the orbits of both planets, as measured by various instruments. The ∼5 yr modulation from 14 Her b is apparent, as is the long-term variation due to 14 Her c, although there is not complete coverage of the outer planet’s orbit.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: Forward modeling of sources in the NIRCam F444W image. (a) Reproduction of the PSF-subtracted image in Figure 1. The two prominent sources are an extended source (a galaxy) to the SE and a point source (14 Her c) to the SW. (b) The residuals after the subtraction of a simple forward model of the background galaxy, a webbpsf point source convolved by a 2D Gaussian. Small (10%) residuals to the SE of the center of the galaxy are apparent. The visual significance of 14 Her c is apparent, as the galaxy has been suppressed. (c) The residuals of the image after the point-source forward model for 14 Her c have been subtracted.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: Posterior distribution on the orbital elements of 14 Her c from the orbitize! orbit fit. Tails on the distributions are correlated with the RV instrumental jitter terms, due to the fractional phase coverage of the observations from various instruments. An additional epoch of JWST/NIRCam imaging will constrain these parameters dramatically by revising the planet’s eccentricity estimate.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: Example dynamical simulations, initialized from different parameter vectors from the orbitize! posterior distribution. The left and right columns show examples of lower and higher amplitudes of secular oscillations, as seen in the eccentricity variations of both planets and the mutual inclination variations. The histogram in the bottom panel shows the distribution of Δeb across all simulations, and the values corresponding to the two example simulations are shown with the vertical red lines.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: Posterior distribution on the orbital elements of 14 Her b from the orbitize! orbit fit. Two solutions for the planet’s inclination ib and longitude of the ascending node Ωb arise due to the ambiguity of the direction of the planet’s orbit.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: The posterior distribution of mutual inclination angles Θ between the orbits of 14 Her b and c, compared to the sine prior. The constraint on the mutual inclination is driven by the likelihood function and not the prior.
Paper: Indication for a Compact Object Next to a LIGO–Virgo Binary Black Hole Merger
Authors: Shu-Cheng Yang, Wen-Biao Han, Hiromichi Tagawa, Song Li, Chen Zhang
Figure caption: Posterior distributions for the primary and secondary masses, luminosity distance, LSA, and nI for GW190814. The contours show the 50% and 90% credible intervals, and the vertical dashed lines mark the median and 90% credible intervals. Notice that the BH masses are given in the rest frame of the source. The waveform template is based on IMRPhenomXPHM.
Paper: Measuring Emission Lines with JWST MegaScience Medium Bands: A New Window into Dust and Star Formation at Cosmic Noon
Authors: Brian Lorenz, Katherine A. Suess, Mariska Kriek, Sedona H. Price, Joel Leja, Erica Nelson, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Pratika Dayal, Anna de Graaff, Jenny E. Greene, Lukas J. Furtak, Ivo Labbé, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Abby Mintz, Ikki Mitsuhashi, Richard Pan, Natalia Porraz Barrera, Bingjie Wang, 冰洁 王, John R. Weaver, Christina C. Williams, Katherine E. Whitaker
Figure caption: Our selected sample of 14 galaxies (large circles) shown with the full UNCOVER sample (gray hexagons) in stellar mass versus SFR (measured by Prospector) and F444W apparent magnitude vs. redshift. Points are color-coded by Hα equivalent width as measured from the prism spectra. Squares show galaxies where the spectroscopic redshift indicates that one of the emission lines is not fully contained in the medium-band photometry. Small circles show objects that do not have high enough Paβ signal-to-noise ratios (SNR < 2) to make accurate emission line measurements. We show the P. Popesso et al. (2023) star-forming main sequence (SFMS) at the mean redshift of our sample, z = 1.96. We see that our sample includes galaxies on both sides of the SFMS. Galaxies are spread across the 1.3 ≤ z ≤ 2.4 range and detected down to 27th magnitude in F444W.
Paper: Measuring Emission Lines with JWST MegaScience Medium Bands: A New Window into Dust and Star Formation at Cosmic Noon
Authors: Brian Lorenz, Katherine A. Suess, Mariska Kriek, Sedona H. Price, Joel Leja, Erica Nelson, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Pratika Dayal, Anna de Graaff, Jenny E. Greene, Lukas J. Furtak, Ivo Labbé, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Abby Mintz, Ikki Mitsuhashi, Richard Pan, Natalia Porraz Barrera, Bingjie Wang, 冰洁 王, John R. Weaver, Christina C. Williams, Katherine E. Whitaker
Figure caption: Images and line maps for each of our 14 objects, sorted by measured photometric AV. First column: RGB image, with the Hα emission line falling in the green medium band and the position of the NIRSpec slit shown in white. We show a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 scale bar, as well the DR3 ID from the UNCOVER public catalogs. Second column: continuum map (measured near Hα) overlaid with Hα emission map contours at signal-to-noise ratios of 1 through 5. Third column: Hα emission line map. Fourth column: the same Hα emission line map overlaid with Paβ map contours at signal-to-noise ratios of 1 through 5. Locations with strong Paβ but low Hα are likely dusty.
Paper: Measuring Emission Lines with JWST MegaScience Medium Bands: A New Window into Dust and Star Formation at Cosmic Noon
Authors: Brian Lorenz, Katherine A. Suess, Mariska Kriek, Sedona H. Price, Joel Leja, Erica Nelson, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Pratika Dayal, Anna de Graaff, Jenny E. Greene, Lukas J. Furtak, Ivo Labbé, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Abby Mintz, Ikki Mitsuhashi, Richard Pan, Natalia Porraz Barrera, Bingjie Wang, 冰洁 王, John R. Weaver, Christina C. Williams, Katherine E. Whitaker
Figure caption:                         We show the Pearson correlation coefficient (r) computed between the Hα emission line map (see Figure 3) and continuum map. We only include pixels that were flagged as part of the galaxy through its segmentation map from UNCOVER. r tends to decrease as photometric AV increases, indicating an offset between the brightest pixels in Hα and the continuum. The offsets suggest that dust is obscuring some of the star-forming regions but not others, indicating patchy dust distribution. They may also hold information about the locations of newly formed stars.
Paper: Measuring Emission Lines with JWST MegaScience Medium Bands: A New Window into Dust and Star Formation at Cosmic Noon
Authors: Brian Lorenz, Katherine A. Suess, Mariska Kriek, Sedona H. Price, Joel Leja, Erica Nelson, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Pratika Dayal, Anna de Graaff, Jenny E. Greene, Lukas J. Furtak, Ivo Labbé, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Abby Mintz, Ikki Mitsuhashi, Richard Pan, Natalia Porraz Barrera, Bingjie Wang, 冰洁 王, John R. Weaver, Christina C. Williams, Katherine E. Whitaker
Figure caption: Comparisons between photometric (y-axis) and spectroscopic (x-axis) measurement of Hα line flux, Paβ line flux, and ﹩\frac{{\rm{Pa}}\beta }{{\rm{H}}\alpha }﹩ ratio for the 14 galaxies in our sample. Points are color-coded by photometric equivalent width in the first two panels and Prospector mass in the right panel. Inferred AV measurements are shown on the right axis of the line ratio plot (right panel). Median offset and 1σ scatter are shown at the bottom right of each plot. Uncertainties are computed from Monte Carlo simulations. We see strong agreement with a scatter of less than 0.15 dex in both lines, demonstrating that the medium bands are a powerful tool for measuring isolated emission lines.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: Top panels: Wi plotted against ﹩{\mathrm{log}}\,(1+z)﹩ for three radial bins (〈D〉 =  0.8 Mpc, 2.5 Mpc, and 5.1 Mpc). The marker shapes denote different elements (e.g., Lyα•, Si▾, O▴, Ni■, etc.), while the colors correspond to their rest wavelengths. Error bars represent 1σ uncertainties in the measurements. Bottom panels: normalized equivalent widths ﹩{W}^{N}=W/1{0}^{\langle \,{\mathrm{log}}\,W\rangle }﹩ as a function of ﹩{\mathrm{log}}\,(1+z)﹩. The gray lines in the lower panels represent a linear fit and its associated uncertainty range. And the colored lines represent fits to specific types of absorption lines based on their tracing gas or the origin mechanisms of the elements, with corresponding slopes and uncertainties indicated in the text of the same color. The observed Wi decreases with increasing redshift, which indicates the enrichment of the gas associated with QSOs.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: Top left: Wi as a function of the impact parameter D for various ions. Different colors and marker shapes correspond to different absorption lines, following the same convention as in Figure 2. The data points are fitted using the halo model (solid line) with a one-halo term (dashed line) and a two-halo term (dotted line). Top right: linear fitting of the observed data; open black diamond markers indicate the Mg II absorption for LRGs as foreground galaxies, as detailed by G. Zhu et al. (2014). The reduced chi-squared values (﹩{\chi }_{\nu }^{2}﹩) for both the halo model and the linear fit are also shown in the figure to compare the goodness of fit between the two models. Bottom left and bottom right: logarithmic ratio ﹩{\mathrm{log}}\,({W}_{i}/{W}_{i}^{\,\rm{model}\,})﹩ of the observed Wi to the predicted values from the model (﹩{W}_{i}^{\,\rm{model}\,}﹩). Error bars indicate the uncertainty of Wi.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: Fitted slopes β for each ion in the ﹩{\mathrm{log}}\,(W)﹩ vs. ﹩{\mathrm{log}}\,(D)﹩ plot (Figure 4) shown as a function of rest wavelength (1200–3000 Å). The colors and marker shapes follow the same convention as in Figure 2. Open black diamond markers represent the Mg II slope from G. Zhu et al. (2014). Projected two-point correlation function slopes of galaxies within the range of 1–5 Mpc are indicated: I. Zehavi et al. (2004) for 0.02 < z < 0.16 (blue), S. E. Nuza et al. (2013) for 0.4 < z < 0.7 (green), and A. Durkalec et al. (2018) for 2 < z < 3.5 (orange).
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: A normalized stacked spectrum of the QSOs. The black curve represents the coadded spectrum, while the blue curve depicts the Gaussian fit to the absorption lines. The shaded gray areas indicate the 1σ errors, and the shaded blue regions correspond to the equivalent widths of the absorption lines. Text labels indicate the names of the corresponding absorption lines and colors matching their rest wavelengths, as shown in the color bar in Figure 2. The plot also displays the redshift range (z > 1.65) and the mean impact parameter (〈D〉 = 5.1 Mpc) of the stacked spectrum.
Paper: The Cosmic Evolution and Spatial Distribution of Multiphase Gas Associated with QSOs
Authors: Zeyu Chen, Enci Wang, Hu Zou, Haoran Yu, Zhicheng He, Huiyuan Wang, Yang Gao, Cheqiu Lyu, Cheng Jia, Chengyu Ma, Weiyu Ding, Runyu Zhu, Xu Kong
Figure caption: Fitted slopes α for each ion in the ﹩{\mathrm{log}}\,(W)﹩ vs. ﹩{\mathrm{log}}\,(1+z)﹩ plot (depicted in Figure 2) shown against a rest wavelength range from 1500 to 3000 Å. The colors and marker shapes adhere to the same convention as in Figure 2. The center of the shaded region represents the average value of α for data points, and the width indicates 2 times the standard deviation.
Paper: Atmospheric C/O Ratios of Sub-Neptunes with Magma Oceans: Homemade rather than Inherited
Authors: Aaron Werlen, Caroline Dorn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Molar bulk atmospheric C/O ratio as a function of atmospheric mass fraction. Dashed lines show results from the reaction network that includes carbon in the metal phase; dotted lines show results from the network excluding carbon in the metal phase. The horizontal dashed lines indicate the initial C/O ratios of the disk and the core. The core C/O ratio is calculated from the initial conditions for the case with C metal. The left panel shows models with an atmosphere–magma ocean interface (AMOI) temperature of 3000 K and a silicate–metal equilibrium (SME) temperature of 3500 K. The right panel shows models with an AMOI temperature of 4000 K and an SME temperature of 4500 K. Including carbon in the metal phase leads to a decrease in the atmospheric C/O ratio at low atmospheric mass fractions.