adsabs/AstroCLIMB huggingface dataset:
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Photometric fit for LSPM J0207+3331. All spectral bands listed in Table 1 are shown with error bars. The best-fit pure hydrogen model (filled circles) is compared to a pure helium model (open circles). Photometric data excluded from the fit are highlighted in red.
Paper: Supra-arcade Downflows in an Extensive Fan Associated with a Giant Quiescent Solar Filament Eruption
Authors: Xiaoyan Xie, Katharine K. Reeves, Chengcai Shen, Nishu Karna, Yan Xu, Christopher S. Moore, Crisel Suarez, Ritesh Patel, Daniel B. Seaton
Figure caption: (a) Snapshot of the giant arches event showing the SAD that has the largest width therein. The arrow indicates the direction of the distance increment. (b) Intensity as a function of distance along the path (white line) marked in panel (a). Orange lines indicate the range of SAD width.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Rosseland mean optical depth at which the monochromatic optical depth reaches τν = 2/3, plotted as a function of wavelength in the vicinity of the Ca II H & K lines for LSPM J0207+3331 (black) and PG 1225−079 (red). This depth approximately corresponds to the layer from which about 50% of the emergent photons at a given wavelength escape, making it a useful proxy for line formation depth.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Dust disk model fit (blue) of the photometric (black) and NIRES (orange) data for LSPM J0207+3331. The white dwarf SED is plotted in gray.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: HIRES data of LSPM J0207+3331 centered around the Ca II K (left) and H (right) lines.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(λ) (top) and P(λ) (bottom) for α = 40° (left) or α = 90° (right) for the four separate views of modern Earth displayed in Figure 2. At α = 90°, the polarization of all four models and the 24 hr integration reach a maximum value of ∼0.5 at λ = 0.4 μm. While the πFn(λ) curves show larger separations in the signals between the different views, the P(λ) curves are affected more by the heterogeneities.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: Our model views of modern Earth throughout its diurnal rotation, with either the Pacific Ocean (left), the Amazon rainforest (middle left), the Horn of Africa (middle right), or Papua New Guinea (right) centered on the disk. The top row shows the surface distributions while the bottom row shows the corresponding cloud distributions we used (see Section 3.2), with cirrus clouds in light blue, stratocumulus clouds in white, and no clouds (i.e., clear atmosphere) in black.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(α) (top) and P(α) (bottom) for λ = 0.5 μm (left) or λ = 0.8 μm (right) for our modern Earth of Figure 2. The planet rotates on its axis once every 24 hr. Variability due to the different surfaces and clouds moving into and out of view lead to the “noise” observed in the 6.67 hr observations (blue circles), while these variable features get smoothed out in the 24 hr observations (red stars).
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: Surface (top row) and cloud (bottom row) distributions for our various Snowball Earth models. The surface was either modeled as a fully ice-covered HS (top left) or contained a tropical ocean belt to simulate an SE scenario (top right). Low-altitude water ice clouds (light blue) could have existed in an equatorial belt during summer months (bottom left) or only in the Southern Hemisphere during winter months. In winter these low-level clouds could have been fully covering the hemisphere (bottom middle left), scattered throughout the hemisphere (bottom middle right), or scattered throughout with additional high-altitude (grayish-blue) water ice clouds (bottom right).
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: Diurnal rotation of our modern Earth scenario observed at three different λ and either α = 40° (left) or α = 90° (right). Snapshots of the surface distributions for each view at both phases are shown in the top images. While the reflected total normalized flux, πFn (top), shows overlapping variability at both phases between the observed bandpasses as the planet rotates, we can see clear separation between observations at α = 90° in the degree of linear polarization, P, curves (bottom).
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: Diurnal rotation light curves of a planet with a Lambertian reflecting ocean, a single large sandy supercontinent, and a clear Proterozoic Earth atmosphere (see K. E. Goodis Gordon et al. 2025) observed at phase angles of α = 90° (circles) or α = 40° (diamonds) at ∼2.7 hr increments. The supercontinent rotating in and out of view leaves clear traces on both the disk-integrated reflected flux, πFn, (top) and degree of linear polarization, P, (bottom) of the planet.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Left: column density ratios, NC IV/NO VI vs. NN V/NO VI—comparison of observations (markers) and ionization models (curves). The curves are shown for CIE (solid) and a few gas densities (dashed, dotted–dashed, and dotted). The color along the curve shows the gas temperature, from 106 K (red) to 104 K (blue). Marker shape indicates the type of constraint on gas properties (see text in Section 4.2.2), and the magenta marker shows the object presented as an example in the right panel. Right: gas density and temperature constraints for a specific object, with limits on both N V and C IV. The gap between the regions allowed by each ratio suggests that the three ions cannot form in the same phase. Black dashed curves show the gas pressure, and dotted—cooling time (for Z = 0.3).
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Observed C IV (left panel; purple circles), O VI (middle panel; orange diamonds), and N V (right panel) component column densities vs. line widths (bD,99.7). The x-axis corresponds to the observed line widths for the data and vcool for the model predictions (bD ∼ bD,99.7 ∼ vcool) in km s−1. We note that we only plot observations with bD,99.7 values ≥10 km s−1. The various lines show the predicted cooling flow column densities at different temperatures, assuming 0.3Z⊙; the solid lines and dashed lines were calculated without thermal broadening taken into account, while the dotted line takes into account thermal broadening for just the peak temperature of each ion. The horizontal line in each panel represents the average upper limit value for the ion presented in the pane,l with the shaded region acting as a visual representation of the possible values these upper limits could be across the range of velocities. The horizontal lines for each ion are as follows: 13.2 for C IV (R. Bordoloi et al. 2014; S. L. Garza et al. 2024) and 13.5 for O VI and N V (J. K. Werk et al. 2013, 2016). The cooling flow models match the O VI and N V observations fairly well, as the data lie between the cooling flow model for T = 105.5−6.0 and T = 105.3−5.8 K for O VI and N V, respectively. However, the C IV observations do not follow the cooling flow model and lie above the model predictions.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Column density C IV, O VI, and N V ratios colored by the sSFR. Top left panel: C IV column density vs. O VI column density. Top right panel: the ratio of C IV column density and O VI column density as a function of impact parameter normalized by the viral radius (Rproj/R200c). Bottom left panel: NC IV/O VI as a function of stellar mass. Bottom right panel: NC IV/O VI vs. the ratio of N V column density and O VI column density (NN V/O VI). These empirical plots showcase the ratios we use to understand the gas properties through Cloudy modeling in Section 4.2. We note that the open circles denote that the top column density or column density ratio value is unconstrained via an upper limit value.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Column density ratios in the gas temperature–density parameter space, for NC IV/NO VI (left) and NN V/NO VI (right). The thick solid contours indicate fixed log10(N1/N2) of the given quantity along each line of sight for the range of ratios observed in the lower right panel of Figure 7 (∼ −1.0–1.0), whereas the dashed contours indicate isobars of the pressure indicated. The magenta solid contour shows the gas cooling/heating equilibrium temperature as a function of density. In Figure 9, we compare our observations to the models shown here.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Normalized distributions of the ratio between the observed C IV, O VI, and N V column densities from the peak temperature cooling flow model (not taking into account thermal broadening, Equation (4)). The normalized distributions are set so that the sum of the counts equals one; the counts per bin (bin width is equal to 0.1) are divided by the number of observations for each ion. We find that on average, C IV is ∼2.5 (log10 0.4) times higher than the model predictions.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Column density ratios for lowered C IV and N V depletion (filled markers). Gray markers show the original measured ratios (see Figure 9) for comparison.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Constraints on gas density and temperature from column density ratios for individual objects. The two example cases are (left panel) the C IV/O VI constraint and (right panel) consistent with single-phase gas (right panel). The first case requires multiphase gas (C IV and N V cannot come from the same phase). Black dashed curves show gas pressure.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Spectra from the CIViL⋆ survey with no prominent absorption features. We denote our upper limit column density estimations in the legend for each sight line. We do not use COS-GASS matched sight lines J1427+2632 (45940), J1502+0649 (41743), and J1544+2740 (28317) for this paper’s analysis.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: These six panels show how various properties of the selected clumps vary with the clump size (proxied by the sphericalized radius) and with clump mass. The figure shows clumps from all six halos aggregated together. Each 2D distribution is color coded separately. The top rows show the properties of the clumps themselves, whereas the bottom panels show the same property but with respect to the clump environment. From left to right, we show the average radial clump velocity (top) and the ratio between the average clump radial velocity and the radial velocity of the clump environment (bottom); the clump pressure (top) and the pressure ratio between clump and environment (bottom); and the clump metallicity (top) and the metallicity difference between clump and environment (bottom). The color bars for the log ratios were chosen to be symmetrical around zero. To give a better idea of the total distribution, the first (99th) percentile of the pressure ratios is −0.6 (0.7) with 8% of the data outside the color bar range. For the metallicity ratios the first (99th) percentile is −1.3 (0.2) with 11% of the data outside the color bar range. Further details are described in the text in Section 3.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: These six panels show how various properties of the selected clumps vary with the clump size (using the sphericalized radius as a proxy) and with clump mass. The figure shows clumps from all six halos aggregated together. Each 2D distribution is color coded separately. From top left to bottom right, we show the number in each 2D bin, the number of gas cells per clump, their distance to the galaxy center, the fraction of satellites in the clump population, the fraction of ISM clumps in the total clump population, and the average H I fraction in each size–mass bin. Further details are described in the text in Section 3.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: The radius (top left), mass (top right), velocity (bottom left), and shape (bottom right) of the clumps. In blue we show the histograms and in orange the kernel density estimate of the same data. For size we use a proxy, the “sphericalized clump radius.” Their minimum size of 0.23 kpc is defined by the minimum size we require in the clump-finding process and the resolution of the simulation. The median size of the clumps is around 0.4 kpc. While the size histogram has a clear cutoff, the mass distribution follows a smooth distribution with no sign of a cutoff, indicating we are not missing a significant amount of mass trapped in unresolved structures. The mass of the average clump peaks around 105 M⊙ and is somewhat more round than filamentary, with a large scatter over possible morphologies. In terms of radial velocity we find that the majority of clumps are slowly moving toward the galaxy, with a few exceptional clumps leaving the galaxy at high velocities.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: Physical properties of an individual inflowing clump. Similar to the outflowing case (Figure 10), we find that the overdense structures show up prominently in the temperature and metallicity plots as a low-temperature, low-metallicity object. In the radial velocity plot we find little distinction between the clump and its environment, suggesting it is well embedded within its surroundings and not experiencing a lot of shear. The H I is well contained within the clump whereas high-ionization ions like O VI show up homogeneously in the projection, as there is little added O VI from the clump structure. In fact, the O VI column densities increase outside the edges, indicating that high-ionization ions trace the diffuse medium and edges of overdense structures rather than the clumps themselves.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: These four panels show how the density and temperature of a subset of the clumps vary with the clump size (proxied by the sphericalized radius) and with clump mass. The figure shows clumps from all six halos aggregated together. Each 2D distribution is color coded separately. The top-left panel shows the number of clumps in each hexbin for this subset. The top-right panel shows the density contrast of the clumps to their ambient medium. The bottom-left panel shows the average temperature in each clump bin and the bottom-right panel shows the temperature contrast. Further details are described in the text in Sections 3.2.7 and 3.2.8.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: Density spread within each of the six FOGGIE halos (colored bars in the background) as well as the chosen minimum detection thresholds when identifying clumps (gray horizontal lines). The violin plots indicate the distributions of densities found in the cells of the identified clumps in each halo. The global minimum threshold is set by Hurricane and the global maximum by Squall.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: Gas density projection maps of the six FOGGIE halos at z = 1. These density projections clearly show clumpy structures throughout the gas halos, concentrated within the inner 40 kpc of the CGM.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: Illustration of the clump-finding process (from upper left to lower right). Starting at lower-density isocontours, coherent structures are identified and within them a higher-density threshold is applied to find “children” structures within the previous one until we arrive at a set of “leaves,” which are the highest-density structures within a certain environment.
Paper: Can Repeating and Nonrepeating Fast Radio Bursts Be Drawn from the Same Population?
Authors: Paz Beniamini, Pawan Kumar
Figure caption: Top: estimated source number densities of different FRB subclasses. These are plotted against the rate per source extrapolated to an intermediate common energy of 1028 erg Hz−1 using the measured γ or γ ≈ 1.7 ± 0.2 when not available. Uncertainties mark the range corresponding to 90% confidence limits. A diamond indicates the same properties for the hypothetical test case (disfavored by our analysis, see Appendix B for details) that a single source type dominates the CHIME data. Since the latter is dominated by nonrepeaters, this also provides a rough estimate for the number density and rate of CHIME nonrepeaters. We find that approximately ﹩{n}_{{\rm{obs}}}\propto {{ \mathcal R }}^{-1}﹩ over a factor of ∼109 in density, suggesting that the large range between common and inactive and rare and active sources might be fit by a single PL distribution with roughly equal contributions at different logarithmic scales. Bottom: rate per source as a function of (proper) distance. Results are shown for extragalactic FRB repeaters and nonrepeaters with well-constrained distances and rates. Downward facing triangles indicate 90% upper limits. Consistency with the PL distribution of activity rates, ﹩{n}_{{\rm{obs}}}\propto {{ \mathcal R }}^{-a}﹩, requires that sources occupy the region below a boundary given by ﹩{ \mathcal R }\propto {d}_{{\rm{p}}}^{3/a}﹩—i.e., within the blue shaded region.