adsabs/AstroCLIMB huggingface dataset:
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: Comparing PH and tight representatives of different samples of original and trimmed data sets at different sampling percentages. (A) The number of significant features in PD and number of tight representatives computed when birth and persistence thresholds were kept the same across all samples (τ  u  = 22.5 h −1 Mpc, ϵ = 7.5 h −1 Mpc). (B) Centroids of computed voids. (C) Results of the Mann–Whitney U rank test for comparing distributions of x, y, and z coordinates of void centroids for all pairwise combinations show that these distributions cannot be statistically distinguished (p-values ≫ 0.05).
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: The number of tight representatives can be smaller than the number of significant features. (A) A simulated data set embedded in ﹩{{\mathbb{R}}}^{2}﹩ with three distinct holes. (B) H1 PD shows there are three features with relatively high persistence. (C) Representatives from the matrix reduction algorithm are shown in black. Their birth parameters are 5.06, 4.98, and 4.41. Tight representatives after greedy shortening (τ  u  = 10) are shown in red. Their birth parameters are 8.23, 5.56, and 9.2. Consequently, they have lower persistence, and some may be classified as nonsignificant depending on the persistence threshold.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Test of the viscosity efficiency in our simulations. A ring of mass m placed in a Keplerian orbit at R = R 0 spreads under the action of viscous torques. The surface density Σ is shown as a function of x = R/R 0 and the dimensionless time variable ﹩\tau =12\nu {{tR}}_{0}^{-2}﹩, with ﹩\nu =\mathrm{const}﹩. The solid curves represent the solutions obtained through our simulations, while the dashed curves are the analytical solutions obtained by J. E. Pringle (1981).
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: (A) A noisy discrete data set with one significant hole. (B) The births and deaths of holes are plotted as a persistence diagram. This example shows that only one hole has relatively high persistence. (C) Representative boundaries tighten as they are shortened by our algorithm. (D) A point cloud in three dimensions. No significant hole is visible. (E) PD shows that one feature has relatively high persistence. (F) Our algorithms improve geometric precision. The blue boundary is the birth cycle from the recursive algorithm. The red boundary is the smooth cycle after applying the greedy shortening and smoothing algorithms.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: Number of H2 features is computed for 50 samples of three different perturbations of the data sets. Different colors show different magnitudes of the perturbation. (A) The mean number of features with persistence at most x decreases exponentially as x increases. (B) The standard deviation in the number of features is small and consistent across the three perturbations for persistence thresholds greater than 7.5 h −1 Mpc (dashed vertical line).
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: (A) Distributions of cycle lengths before and after greedy shortening at different birth thresholds (τ  u ). The distributions are similar for τ  u  > 17.5 h −1 Mpc. (B) The number of significant features around which we can find a representative after greedy shortening attains a maximum at τ  u  = 22.5 h −1 Mpc.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: The angular distribution of SDSS galaxies on the sky. In the Appendix, we cut the gold points from the sample and reanalyze the data to test the sensitivity of the void properties to the boundary.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: Computation times and memory for different under samples of the SDSS data set.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Comparison of the variation in the outer disk radius from our simulations with the observational results of R. Baptista & M. S. Catalán (2001). Upper panel: The points with error bars are the measurements of R. Baptista & M. S. Catalán (2001), while the red and blue lines represent the case of local emission by blackbody and gray atmosphere, respectively—with the solid line being the outer disk radius and the dashed line being the radius of stream penetration. The black dashed and dotted lines mark the value of the circularization radius and the minimum radius of S. H. Lubow & F. H. Shu (1975), respectively. Bottom panels: The residuals of each fit.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Best-fit simulation in the case of local emission by gray atmosphere. The notation is similar to that of Figure 10.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Density (a), temperature (b), vorticity (c), and radial velocity (d) evolution in vortex-forming disk (σ  ϕ  = 0.236, ϵ = 0.5, α = 0, β = 0.001, p = −1.0). The color ranges for density, vorticity, and radial velocity differ between the early spiral formation stage (first and second rows) and the vortex-dominant stage (third and fourth rows). The simulation duration increases sequentially from top to bottom. The white frame delineates the boundary of each identified vortex, and there are no significant structures inside the white frame in the temperature plot (b) (compare with density (a), vorticity (c), and radial velocity (d)) due to rapid cooling. A white star within each frame indicates the center of the vortex. The red numbers highlight the selected vortices.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Statistics of shadow-driven substructures based on 80 of 160 simulations with constant disk aspect ratio (h = 0.1). The figure is divided into two parts by a dashed line, representing the shadow width being 45° on the left and 15° on the right. Within each part, the left column corresponds to disks with ϵ = 0.5, while the right column corresponds to disks with ϵ = 0.8. Each subfigure in the β–α sections represents a specific combination of parameters. Within each β–α section, there are three rows representing the dominant structures in the disk: vortices/crescents, rings, and spirals from top to bottom. Each type of structure is represented by a different type of square marker, whose color represents the density contrast of the substructures. Examples of dominant substructures are shown in the row with α = 10−3 in the leftmost subfigure (σ  ϕ : 0.236, p: −1, ϵ: 0.5), with “S” indicating spiral-dominant, “R” indicating ring-dominant, and “V” indicating vortex-dominant. The figure also includes red and blue line shaded areas, indicating disks undergoing transitions from vortex−ring and ring−spiral phases, respectively.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Density (a), temperature (b), radial velocity (c), and azimuthal velocity (d) evolution in spiral-forming disk (σ  ϕ  = 0.236, ϵ = 0.8, α = 10−3, β = 10, p = −1.0). All quantities except for v  r  are normalized by their initial values, and v  r  is normalized by initial v  ϕ . The color range for temperature differs between the formation process of the early stage (first and second rows) and the relative quasi-steady state (third to fifth rows). The white solid lines represent the fitted spirals based on density contrast.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Density (a), temperature (b), radial velocity (c), and azimuthal velocity (d) evolution in ring-forming disk (σ  ϕ  = 0.236, ϵ = 0.5, α = 10−4, β = 1, p = −1.0). All quantities except for v  r  are normalized by their initial values, and v  r  is normalized by initial v  ϕ . The black dashed lines represent the fourth and fifth fitted rings in this disk.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Density (a), temperature (b), radial velocity (c), and azimuthal velocity (d) evolution in linear evolution disk (σ  ϕ  = 0.236, ϵ = 0.001, α = 0, β = 0.001, p = −1.0). All quantities except for v  r  are normalized by their initial values, and v  r  is normalized by initial v  ϕ .
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Normalized density perturbation for simulations with Ωshadow = 1Ω0 (a), 0.03Ω0 (b), and 0.003Ω0 (c) at the final steady state under the parameters setting as σ  ϕ  = 0.236, ϵ = 0.001, α = 0, β = 0.001, p = −1.0. The radii of corotation resonances, inner Lindblad resonances, and outer Lindblad resonances are shown as yellow, green, and purple dashed lines, respectively.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: The average and error of normalized vortex/crescent spacing. The black solid line represents simulations with p = −1.0, while the red solid line represents simulations with p = −0.5. Points marked with an “x” do not have error bars. In this case, there are at most two selected vortices/crescents within the disk. The upward arrows represent lower limit points, where there is only one selected vortex/crescent within the disk.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Formation processes of substructures from linear to nonlinear regimes. All plots show the density contrast in disks in logarithmic scale.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: The average and error of normalized ring spacing. The black solid line represents simulations with p = −1.0, while the red solid line represents simulations with p = −0.5. Points marked with an “x” do not have error bars. In this case, there are at most two selected rings within the disk. The upward arrow represents lower limit points, where there is only one ring within the disk.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Distribution of the angle between the orbital pole of a satellite galaxy and the coorbiting GPOA normal vector, based on 105 Monte Carlo samplings from the measurement uncertainties. The dashed lines indicate the angle inferred from the most likely values, while the dotted lines indicate the 1σ spreads. Since the spatial position of And III is offset by 21.°5 from the GPOA, this is the minimum angular alignment that is geometrically achievable for its orbital pole.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Spatial distribution of satellite galaxies around M31. Upward/downward triangles mark those satellites with receding/approaching line-of-sight velocities relative to that of M31. Filled symbols mark the candidate members of the GPOA according to their line-of-sight velocities and spatial distribution, with red/blue color also indicating the receding/approaching satellites. The GPOA and its estimated width are highlighted with dashed and dotted lines, respectively. The on-sky velocities relative to that of M31 for NGC 147, NGC 185 (S. T. Sohn et al. 2020), and And III (this work) are marked with green arrows.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: Distribution of calculated orbital poles of And III relative to M31 from 105 Monte Carlo realizations, in Galactic coordinates. The orbital pole corresponding to the most likely measured position and velocity is shown as a red cross, the peak in the density distribution as a magenta circle. The blue plus sign indicates the normal vector to the GPOA that corresponding to the direction of corotation inferred from the line-of-sight velocity coherence, while the black diamond indicates the spin of the galactic disk of M31. See Figure 2 in M. S. Pawlowski & S. T. Sohn (2021) for equivalent plots for the two other M31 satellites with measured proper motions, NGC 147 and NGC 185.
Paper: HST Proper Motion of Andromeda III. Another Satellite Coorbiting the M31 Satellite Plane
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
Figure caption: The M31-centric distance and total velocity of And III (black) using the HST + Sats M31 proper motion (square) and its weighted average with EDR3 (diamond). Escape velocity curves of the two M31 mass models adopted in this paper are shown in blue and red, while a Milky Way–like potential is displayed for reference (gray dashed line). Results for NGC 147 and NGC 185, two other M31 satellites with proper motions, are also shown in purple and orange, respectively.
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: Twist rate α (left-hand panels) and the radial curvature  B  · ∇(B  r )/B 2 (right-hand panels) in the vertical cross section (whose location is indicated by the black line in Figure 6(a)) across the middle of the central PIL at the time of the onset of the first eruption (top) and at a time during the eruption (bottom), overlaid with arrows that show the direction of the magnetic field within the cross-section plane, and also overlaid with the contours of the decay index ﹩d(\mathrm{ln}{B}_{p{\rm{h}}})/d(\mathrm{ln}h)﹩, where B  ph is the horizontal field strength of the corresponding potential field and h denotes the height above the lower boundary surface.
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: A 3D view of example field lines before (left-hand panel) and after (right-hand panel) undergoing tether-cutting reconnections. Field lines are colored in the twist rate α and the gray scale image shows the normal magnetic field B  r  in the lower boundary.
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: Upper panels show AIA 211 Å channel images at the onset of (a) and during (b) the eruption, and the difference image (c) between the two. Lower panels show the lengths of the field lines traced from each location at the base of the corona at the onset of the eruption (d) and at a later time when the outer erupting flux rope is exiting the domain (e), and the change of field line lengths between the two times (f). Three black arrows mark the locations of the major EUV dimming regions observed. The regions marked by the two short arrows correspond to the core dimmings and the region marked by the long arrow corresponds to a more diffuse secondary dimming (e.g., K. Dissauer et al. 2018). Contour lines in the bottom panels show the radial magnetic field on the photosphere, with solid (dotted) contours corresponding to positive (negative) radial fields.
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: (Left-hand panel) The change of the horizontal magnetic field strength ΔB  h  at the lower boundary 12 minutes after the onset of the first eruption in the simulation. (Right-hand panel) The observed change ΔB  h  in the photosphere vector magnetograms 12 minutes after the onset of the observed X-class flare. The black lines are contours of the normal magnetic field B  r  with solid (dotted) lines corresponding to positive (negative) B  r .
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: The observed photospheric horizontal components of the magnetic field B  θ  (a) and B  ϕ  (b) compared with the lower boundary B  θ  (c) and B  ϕ  (d) resulting from the simulation at the time of the onset of the simulated eruption.
Paper: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
Authors: Yuhong Fan, Maria D. Kazachenko, Andrey N. Afanasyev, George H. Fisher
Figure caption: (Left-hand panel) A running difference image from the STEREO-B EUVI 171 passband images of times 01:52:15 UT and 01:53:30 UT on 2011 February 15 during the observed CME eruption. (Right-hand panel) The running difference of two synthetic images in the AIA 171 passband but as viewed from the STEREO-B perspective at times t = 1.555 hr and t = 1.565 hr during the simulated eruption.
Paper: Hydrodynamical Simulations of Proton Ingestion Flashes in Type I X-Ray Bursts
Authors: Simon Guichandut, Michael Zingale, Andrew Cumming
Figure caption: Evolution of the temperature as a function of the column depth (note that the x-axis is reversed), at intervals of 10 ms. The colors get darker as time increases. The labeled and thicker lines are the three times from Figure 3. The circle and square markers show the convective boundaries according to the Schwarzschild and Ledoux criteria respectively. The vertical dotted line is the depletion depth, i.e., the depth of the hydrogen layer. As convection approaches this line, the Schwarzschild and Ledoux boundaries begin to separate. The inset zooms into the evolution near the hydrogen boundary.
Paper: Hydrodynamical Simulations of Proton Ingestion Flashes in Type I X-Ray Bursts
Authors: Simon Guichandut, Michael Zingale, Andrew Cumming
Figure caption: Bulk properties of the flow around the interface between the convective and stable zone prior to the collision, i.e., a moment where this boundary is below the hydrogen layer (at a column depth y > y d, the vertical blue line). In each panel, the solid black line and the color dashed lines are scaled on the left-hand and right-hand sides, respectively. Every quantity is horizontally averaged over the domain and each height. Overbarred quantities are time-averaged over 2 ms. Top: temperature profile and burning rate. Middle: rms velocity fluctuation and adiabatic excess. The crossing of the dashed orange with zero sets the location of the vertical orange line (Schwarzschild boundary). Bottom: convective heat flux and composition fluxes of 1H and 12C.
Paper: Hydrodynamical Simulations of Proton Ingestion Flashes in Type I X-Ray Bursts
Authors: Simon Guichandut, Michael Zingale, Andrew Cumming
Figure caption: Top: evolution of the nuclear luminosity (Equation (4)) with time, for helium burning and metal burning reactions (including CNO), and the total. The production of the most important CNO rates is plotted in dashed lines. Bottom: size of the convective and semiconvective regions as a function of time. The dotted line shows the depletion depth.
Paper: Hydrodynamical Simulations of Proton Ingestion Flashes in Type I X-Ray Bursts
Authors: Simon Guichandut, Michael Zingale, Andrew Cumming
Figure caption: Initial model from MESA (dash-dotted lines), and the initial model A fed into the fluid simulations (solid lines). The top panel shows the temperature profile as a function of the height. The bottom panel shows the composition profiles of the main chemical species, where the green color combines all CNO species. The offset in the position of the solar layer is due to the temperature kick given to the initial fluid model. An alternate initial model (model B) including deep carbon is shown in the dotted lines for CNO and helium mass fractions. See the Appendix for details.
Paper: Hydrodynamical Simulations of Proton Ingestion Flashes in Type I X-Ray Bursts
Authors: Simon Guichandut, Michael Zingale, Andrew Cumming
Figure caption: Illustration of the temperature profile considered for the toy model. In each zone demarcated by the vertical dotted lines (except for the isothermal substrate at large depths y > y base), the best-fitting temperature gradient ﹩{\rm{\nabla }}=d\mathrm{ln}T/d\mathrm{ln}y﹩ is obtained from the MESA model. This temperature profile is then fed into a hydrostatic solver, which determines the density at every point, while the composition is an analytical function of the pressure with Equation (A1). See the text for further details.
Paper: Hydrodynamical Simulations of Proton Ingestion Flashes in Type I X-Ray Bursts
Authors: Simon Guichandut, Michael Zingale, Andrew Cumming
Figure caption: Peak values of the temperature (left axis, solid lines) and Mach number (right axis, dashed lines) as a function of time for the same burst at different resolutions.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Illustration of the power flow in and out for a two-port device simulation in CST, reproduced from the CST’s user help guide. For a single-port device, as is the case for all the antennas considered in this study, the extra port on the right is terminated without outgoing power, with only reflected outgoing power from the input port on the left.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: 68% and 95% confidence contours resulting from fitting our mock beam-weighted foreground spectrum to the patch antenna. We show only the covariances between the regolith dielectric constant, ϵ, and the spectral index parameters, β  j .