adsabs/AstroCLIMB huggingface dataset:
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Metal retention in the cool (blue) and warm (orange) gas phases in the CGM (r > 0.15R200c). The total CGM retention is shown as black bars and gray shaded regions. Shown are the median values for galaxies binned by stellar mass; the error bars/shaded regions denote the 16th–84th percentile range in that bin. We find similar fractions (5%–10%) are retained in the cool and warm phases, and across stellar masses a relatively consistent fraction is retained in the two phases and total CGM.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Column density profiles for all galaxies in the M+M  sample. Each panel shows the median column density profiles in a given ion around a galaxy within the stellar mass bin, denoted at the top of the figure. Each line represents the profile for a single galaxy, color-coded red if the galaxy is from the Marvel suite or blue if the galaxy is from the Massive suite. Also shown is the 16th–84th percentile range for a given galaxy. We find that the overall differences between the two suites are minor.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Fractional extent of the galaxy disk based on three different definitions: the radius at which the surface density of H I  falls below 1.0 M⊙ pc﹩{}^{-2}\,({r}_{\,{{\rm{\Sigma }}}_{\,\rm{HI}\,}=1.0}﹩; blue, the same definition used for ﹩{r}_{\,{{\rm{\Sigma }}}_{\,\rm{HI}\,}}﹩), the radius at which the surface density of H I  falls below 0.5 M⊙ pc﹩{}^{-2}\,({r}_{\,{{\rm{\Sigma }}}_{\,\rm{HI}\,}=0.5}﹩; orange), and the radius within which 90% of the starlight is contained (r90%Light; green). Solid lines show the median values, shaded regions encompass the 16th–84th percentile range, and individual halos are shown as points.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Same as Figure 13 but for Si IV, C IV, and O VI.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Distribution of the SS summary statistics for the identified VAE clusters compared to that of the true phase distribution from the F23 simulation. The top left and right panels correspond to power and sparsity, while the bottom panels correspond to filamentarity, as specified by Equations (7)–(9). The three distinct components identified by the VAE model agree very well in the SS representation with the CNM, WNM+UNM, and noise, respectively.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Image realizations synthesized from the SS representations identified by the VAE model from the F23 simulation data set, compared to the ground-truth synthetic CNM, WNM+UNM, and noise patches. The left panels are the ground-truth synthetic H I images while the right panels correspond to the SS+VAE synthesis. The top, middle, and bottom rows correspond to CNM, WNM+UNM, and noise, respectively. All images are normalized to have zero mean and unit standard deviation.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Result of SS+VAE CNM separation performed on the F23 simulation data set compared to the true CNM distribution for a few different velocity channels of a sample sightline. Left: original synthetic H I emission. Middle: true CNM column density. Right: CNM column density predicted by the SS+VAE model. The last panel shows the pixel-by-pixel correlation between the true and predicted CNM column density, with the white dashed line indicating a one-to-one correlation.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: A flow chart describing the data-driven, morphology-based phase separation framework. The method is composed of a feature-extraction step where we compute the SS statistics of H I emission channel maps I(x), reducing the input into a more compact but still interpretable representation; a feature-clustering step utilizing Gaussian-mixture VAE to learn a component-by-component statistical model of H I phases from the SS statistics; and finally, a component-separation step where VAE outputs are used as priors to inform phase separation via gradient descent synthesis.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Ionization fraction of the simulation volume over time for Aeos10, Aeos20, and the comparison simulations using the Aeos10 Population III IMF but without individual stellar feedback. The shaded gray region shows the 16th to 84th percentile of ionization fractions for the different comparison simulations. Aeos20 ionizes the volume significantly earlier than Aeos10 due to the more massive Population III stars producing more ionizing photons. The comparison simulations have similar ionization to Aeos10, as expected, with stochastic differences beginning to cause large variations between simulations after around 250 Myr. The choice of Population III IMF significantly affects the ionization and consequently the growth of the smallest galaxies.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Median stellar chemical abundances ([X/Fe]) of the oldest low-mass Population II stars from each halo that has started Population II star formation in the simulation, with 16th to 84th percentile scatter between the different halos. The mass of Population III stars affects their yields, affecting the abundances in first-generation Population II stars. In particular, light elements (C, N) and α-elements (O, Mg) are increased in the yields of higher-mass Population III stars, and elements with even atomic numbers (e.g., Mg) are more abundant relative to odd-numbered elements (e.g., Na). The scatter between halos is significant compared to the differences due to the adopted Population III IMF, however.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Mass–metallicity relation for galaxies in Aeos10, Aeos20, and the comparison simulations at z = 14.5. The shaded regions represent the 16th to 84th percentile scatter.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Stellar masses (left) and halo masses (middle) of star-forming halos in the different simulations. Aeos10 has many more small star-forming halos than Aeos20. This is due to higher ionization in Aeos20 (see Figure 1). The distribution of halo masses for all halos (right) in all simulations is nearly identical, as expected.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Starting after ∼150 Myr, Aeos20 (maroon) begins to exceed Aeos10 (blue) in the total ionizing luminosity from Population III stars. This excess of ionizing photons is primarily due to the luminosity of stars greater than 100 M⊙, because when the contribution of these stars is removed (dotted red), the total luminosity of the two simulations is far more similar.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Cumulative fractions of carbon-enhanced metal-poor (CEMP) stars as a function of metallicity. The top panel shows CEMP stars with [C/Fe] > 0.7, and the bottom panel shows CEMP stars with [C/Fe] > 1.0. The low-mass Aeos10 stars are shown as a teal line, the low-mass Aeos20 stars are shown as a maroon line, observations from V. M. Placco et al. (2014) are shown as diamonds, and observations from J. Yoon et al. (2018) are shown as circles. The Population III IMF significantly affects the fraction of CEMP stars, and neither of the Aeos10 nor Aeos20 IMFs reproduces Milky Way observations.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Cumulative star formation history of the full domain down to redshift z = 14.5. Top: population III and Population II star formation of the Aeos10 volume as compared to the star formation of the comparison simulations (without individual Population II star particles or individual feedback). The shaded gray regions show the 16th to 84th percentile scatter between all comparison simulations. Bottom: total cumulative star formation for Aeos10, Aeos20, and the comparison simulations. These bulk properties of the galaxies are not significantly affected by the inclusion of individual stars and stellar feedback.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Comparing the star-forming halos in Aeos10 with those in a typical comparison simulation. The stellar-mass distributions differ; the comparison simulations generally form more galaxies around ∼1000 M⊙. This is because in the comparison simulations, the Population II stars form in particles of 1000 M⊙, biasing any halo that has begun Population II star formation to contain at least 1000 M⊙. The halo mass distributions are more similar because the dark matter modeling is the same between simulations.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Distribution of Population III star masses in Aeos10 vs. Aeos20. Aeos10 has far more low-mass Population III stars, while Aeos20 has fewer total Population III stars, but their masses extend up to 300 M⊙. The black line shows the number of H I ionizing photons from each star as a function of stellar mass; several dozen Population III stars with >100 M⊙ in Aeos20 result in a large number of ionizing photons.
Paper: Determining the 3D Dynamics of Solar Flare Magnetic Reconnection
Authors: Joel T. Dahlin, Spiro K. Antiochos, Peter F. Wyper, Jiong Qiu, C. Richard DeVore
Figure caption: Illustration of the physical connection between a plasmoid and its topological imprint on the solar surface at t = 13,340 s. Panel (a) shows two field-line strips traced from a small-scale spiral on the solar surface L-map (grayscale) to a flare current sheet plasmoid (blue oval in a longitude cut ϕ = 8﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 of the guide field). The vertical current at the solar surface (Jr, green-brown colormap) as well as the flare arcade (light blue field lines), the CME flux rope (magenta field lines), and the PILs (yellow) are shown for context. The green field-line strip was traced from the light gray region of the spiral (shorter field lines) and maps to a conjugate region in the positive polarity region, whereas the orange field-line strip was traced from the dark gray region (longer field lines) and wraps once about the CME flux rope, mapping to a region along the flux rope hook in the positive polarity region. Panel (b) shows a zoomed-out view of (a) illustrating the location of the plasmoid within the eruptive flare/CME configuration. Panel (c) shows a zoomed-in view of the solar surface L-map patch and the footpoints of the orange and green field-line strips. The temporal evolution of the guide field cut and the L-map patch is shown in Figure 10.
Paper: Determining the 3D Dynamics of Solar Flare Magnetic Reconnection
Authors: Joel T. Dahlin, Spiro K. Antiochos, Peter F. Wyper, Jiong Qiu, C. Richard DeVore
Figure caption: Three-dimensional plasmoid structures in the flare current sheet. (a) Context image showing contours of the vertical current density at the inner boundary, illustrating the flare ribbon locations. Yellow field lines indicate the location of the erupting CME flux rope. Five 2D slices of the flare current sheet are also shown, with a color table indicating the guide magnetic field component (Bϕ); concentrations of the guide field indicate plasmoids. Panels ((b)–(f)) show distinct sets of field lines traced from the slices indicated in panel (a), illustrating the twist and topology of the plasmoids. Examples of plasmoids sunward and antisunward of the flare reconnection X-line are shown in (g) and (h), respectively.
Paper: Determining the 3D Dynamics of Solar Flare Magnetic Reconnection
Authors: Joel T. Dahlin, Spiro K. Antiochos, Peter F. Wyper, Jiong Qiu, C. Richard DeVore
Figure caption: Three proxies for flare ribbons. (a) Squashing factor (Q), denoting strong gradients in magnetic field connectivity. (b) Vertical current density (Jr, marking the footprints of the flare current sheet on the solar surface). (c) Field-line length maps, indicating distinct topological regions associated with discontinuous, contrasting field-line lengths. (d) A simple proxy for flare ribbons given by ΔL(t) = L(t + 10) − L(t − 10).
Paper: Determining the 3D Dynamics of Solar Flare Magnetic Reconnection
Authors: Joel T. Dahlin, Spiro K. Antiochos, Peter F. Wyper, Jiong Qiu, C. Richard DeVore
Figure caption: Three-dimensional volumetric visualization of the total current density in the flaring region at t = 13,400 s. Magenta indicates the most intense currents. Grayscale color table indicates the radial component of the magnetic field at the inner boundary of the domain, and yellow curves indicate polarity inversion lines. Orange field lines trace the erupting magnetic flux rope.
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: SNEC model luminosities and photospheric velocities (colored curves) plotted together with the observed data (black circles). The observed velocities, derived from the Fe II λ5189 feature, were decreased by 600 km s−1 to account for the difference between the optical depths of the observed feature and the photosphere (see text). The model IDs are shown in the legends.
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: Top panel: the density distribution of the various M11-csm models listed in Table 2. Note that the distance from the outmost surface of the CSM envelope (in cm) is plotted on the horizontal axis due to the convention used by SNEC. The innermost part of the SN envelope is omitted for display purposes. Bottom panel: the luminosity evolution of the various M11-csm models (colored curves) compared with the observations (red symbols). The LC from the M11 model without the CSM (dotted curve) is also shown for comparison.
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: The bolometric LC of SN 2023ixf plotted together with the semianalytic LC2 model shown in Table 1. The top panel shows the data with the combined (core+shell) model, while the bottom panel displays the core and shell components separately, as well. See text for explanation.
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: The same as Figure 3 but for SN 2017eaw. The dashed line in the upper panel represents the model without the energy input from the magnetar.
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: Comparison of the observables from SNEC (symbols) and from STELLA (curves) against the kinetic energy E51. The dashed lines indicate the observed values for SN 2023ixf.
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: The observable parameters from SNEC models (see Table 3) compared with the observed values of SN 2023ixf (asterisk).
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: The effect of the extended Ni-distribution (model M15o-ni, plotted with blue dashed line) on the light curve (top panel), and on the velocity curve (bottom panel) compared with the observations (black circles) and the M15o-csm1 model (red lines).
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: Demonstration of how parent body compositions at a given accretion phase are assessed for agreement with chondritic abundance ratios. Here the mass-buildup accretion phase is shown for two WDs in our sample. G29–38 is the coolest H-WD in our sample and the only such object that could plausibly be in the mass-buildup phase (T. Cunningham et al. 2022; settling timescales between 1.8 and 6.5 yr; the next coolest H-WD is WD 0145+234 with <2 week settling timescales as reported in Table 3). Ratios are relative to Mg and normalized by CI chondrite abundance ratios. The ﹩{\chi }_{\nu }^{2}﹩ goodness of fit of the abundance ratios to CI chondrite is listed in the upper right corner, and the error bars show the 2σ uncertainties used to calculate ﹩{\chi }_{\nu }^{2}﹩. Only the lithophile elements (outlined in black) are included in the ﹩{\chi }_{\nu }^{2}﹩ calculation.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: Abundances of the observed H-WDs described in Section 2 assuming the steady-state accretion phase, ratioed to Mg and reported relative to CI chondrites with 2σ uncertainties. The circular points show values determined from optical spectra, while the squares show the UV results. All points are colored according to the corresponding element. For clarity, we show only the detection of WD J0649−7624’s O abundance in the photometric and spectroscopic solutions.