adsabs/AstroCLIMB huggingface dataset:
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: (Left) The (GBP − GRP, G) CMD of crossmatched red supergiants, yellow supergiants, and Wolf–Rayet stars from the B10 catalog. The 87 red supergiants are represented by red triangles, the 441 yellow supergiants by yellow Y-shaped symbols, the 8 WN-type stars by green crosses, and the single WO-type star by a green star symbol. The black circles represent the 7426 massive star candidates identified in this study. The area above the magenta line represents the selected region for massive stars. (Right) The (GBP − GRP, G) CMD of crossmatched B1-type stars, B2-type stars, and other later B-type stars (B3–B9) from the B10 catalog. The 186 B1-type and B2-type stars are represented by cyan Y-shaped symbols, while the other later B-type stars are represented by blue triangles. The black circles represent the 7426 massive star candidates identified in this study. The area above the magenta line represents the selected region for massive stars. The red arrow represents the reddening vector corresponding to AV = 0.30 mag.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: The (GBP − GRP, G) CMD after excluding foreground objects from the newly defined circular SMC region and the symmetric region with respect to the Galactic plane. The region above the magenta line is the area occupied by massive stars in the CMD, defined in Section 2.1. Stars contained within the SMC region are represented by black circles, while stars from the symmetric region are represented by green crosses.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: The median internal PMs and the mean RVs of the nine superstructures identified by DBSCAN. The vectors extending from each superstructure represent the median internal PMs, with the scale represented by the legend corresponding to a PM vector magnitude of 30 km s−1. The colors of each superstructure represent the mean RVs after subtracting the systemic RV of the SMC, which is 160 km s−1.
Paper: Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates
Authors: Satoya Nakano, Kengo Tachihara, Mao Tamashiro
Figure caption: Nine superstructures identified using DBSCAN. Different structures are distinguished by color and numbers.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: Scheme for one hydrodynamic cycle in Kratos, showing the parallelization pattern and the interface calls for data exchange. Each “rank” denotes a process, typically controlling one GPU, on which the calculations for multiple blocks are conducted. Each row (labeled by the “Block X, Stream sX” at the beginning of each row) denote the numerical processes of one block on the 2d-tree mesh, which are located on one GPU stream for proper data synchronizations. Different steps of the Godunov solver are marked by colors (red for the preparation of primitive variables, green for calculation of the Riemann fluxes, and magenta for the updates of conservative variables), while the communication operations are marked with blue. Black solid blocks stand for the synchronizations of each stream, taking place within the calls of communication operations to minimize waiting and thus maximize the efficiency.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: The L1 errors in the convergence tests for the default hydrodynamic module in Kratos (see also Section 4.1). The top panel shows the sinusoidal sound wave tests, comparing the results with different computational precisions with the L1 ∝ N−2 power law. The lower two panels exhibit the results for contact waves and shear waves with top-hat and sinusoidal initial conditions, respectively, using the mixed-precision methods (see also Section 3.2.2; note that full-double-precision results are almost identical to the mixed-precision ones, and are thus not illustrated).
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: The overall structure of the Kratos code. Based on the abstraction layer for computing devices and the abstraction layer for the mesh structures, the module container holds all capable modules for physical processes taking place in astrophysical simulations (hydrodynamic module elaborated in this paper, other modules will be described in forthcoming papers; L. Wang 2025, in preparation). While complicated physical calculations can be constructed through the interactions of modules, a user interface (problem generator) handles the definition of initial, boundary, and in-simulation conditions. Such interface can also handle the initial conditions defined by a Python-based interface. Actual astrophysical objects and processes are simulated based on all fundamental systems described above.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: Restriction and prolongation operations near the block refinement interface. Colors are used to mark the corresponding relations across the interface separating coarser (left) and finer (right) blocks. The prolongations are computed on the coarser side, and the x-derivatives qx,I,J are calculated using minmod slope limiter in a pattern indicated on the coarser mesh (derivatives along other directions can be obtained similarly).
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: Boundary condition methods for hydrodynamics, showing four normal columns as examples to illustrate how Kratos rotate the normal columns to the x-direction to unify the methods on the interfaces of block boundaries. Colors indicate the corresponding cells before and after the rotations.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: Patterns of calculating the fluxes for hydrodynamics, illustrating the utilization of shared memory. All processes within the middle dashed box use the shared memory instead of the global memory, as the memory-related operations are frequent, and the data in each cell is typically used many times by multiple threads (indicated by the braces and blocks in the middle box).
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: The method that Kratos handles the interaction of different physical processes via sharing the data held by modules. An instant data structure, encapsulating the shallow copy of all data needed held by all relevant modules, is created as a data proxy right before the launching of each GPU job conducting the calculations.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: Results of the tests on colliding outflows and ambient gases, showing the mass density profiles at t = 1 (top row) and t = 2 (middle row) for low resolution (Δx = 1/32; left column), static mesh-refinement (SMR) with mixed-precision (equivalent Δx = 128; middle column), and SMR with full-double-precision (right column) cases. Block boundaries are indicated in related panels to illustrate the mesh layouts. The bottom row illustrates the Hilbert curves generated for the job dispatching and load balancing for the uniform grid (left panel) and SMR (middle panel) simulations, where the lines connecting blocks on different levels are shown in different colors, and cross-level connections are indicated by dashed lines. The evolution history for the acceleration on the central object of the three different simulations (lower right panel).
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: Scaling performance on multiple GPUs on different types of devices (RTX 3080 and RTX 4090), with mixed-precision and full-double-precision methods respectively. Tests are based on the outflow–incoming flow interactions (see Section 4.7 and Figure 13). The upper panel shows the strong scaling (with the same total computation load), and the lower panel is for the weak scaling (with the same computation load per device).
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: The Kelvin–Helmholtz instability tests results, comparing the t = 1.2 (upper row) and t = 2.4 (lower row) for the uniform grid (left column) and static mesh-refinement (SMR; middle column) results for the relative difference (right panel) in mass density. The block boundaries are indicated in the panels for the SMR simulation, showing the mesh-refinement results (note that each block has the same number of cells).
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: Results of double Mach reflection tests, using mixed-precision (top panel) and full-double-precision (middle panel) methods. The 30 contour lines starting from ρ = 1.73 to ρ = 2.1 are spaced evenly in ρ, indicating almost identical patterns on these panels. The bottom panel illustrate the relative differences of mass density comparing the top two panels.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: The Liska–Wendroff implosion tests results, showing t = 0.045 (upper row) and t = 2.5 (lower row), comparing the mixed-precision (left column) and full-double-precision (right column) methods. Contours span from ρ = 0.35 to ρ = 1.1, spaced evenly by δρ = 0.025.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: The 1D tests of Sod shock tubes, showing the results of cases 1–5 and 7 in E. F. Toro (2009) using the original setups and parameters. The exact semianalytic solutions are indicated by dashed lines, in the same color for the corresponding physical quantities of Kratos numerical calculation results. All calculations in these tests use mixed-precision methods.
Paper: The Kratos Framework for Heterogeneous Astrophysical Simulations: Fundamental Infrastructures and Hydrodynamics
Authors: Lile Wang
Figure caption: The Rayleigh–Taylor instability tests, showing t = 2, 3, and 4 results in three columns for the simulations on uniform grid (top row) and with mesh refinement (bottom row). Similar to Figure 11, the block boundaries are indicated to illustrate the mesh-refinement layouts.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: Left panel: dust surface and ice mantle sputtering rate coefficients versus time for different models. Right panel (MC1 model): the abundances of H2O, CO, and CO2 molecules change with time.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: The schematic diagram depicts the multiphase model. The yellow area represents the gas phase. The blue circles represent the active layer molecules, capable of freely diffusing and undergoing reactions. The green circles depict the normal species within the frozen ice mantle, which are unable to diffuse. The red circles represent the interstitial species, capable of diffusion and reacting with both interstitial and normal species. The presence of light blue circles indicates that the molecules have been excited by cosmic rays, resulting in an excited state that enables them to react with neighboring molecules. Cosmic rays can cause molecules, including those in interstitial and normal species, to be sputtering into the gas phase.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: Abundance ratios of gas species relative to H in different models.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: Abundance ratios of dust species relative to H in different models.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: The distribution of Fempty in different ice layers of the MC2 and MC6 models at 106 yr.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: Abundance ratios of gas carbon-chain species relative to H in the MC1 and MC6 models.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: H-R diagram of the initially selected sample. The colors of the points indicate the [Fe/H] from the included sources, reflecting their metallicity, as coded on the color bar to the right. The H-R diagram is partitioned into four distinct regions by the solid red lines: Dwarf, RC–HB, Giant I, and Giant II (see the text).
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: Abundance ratios of gas carbon-chain species relative to H in the MC2 and MC2_reacDes models.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: The cumulative probability of different desorption mechanisms in various models.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: The fraction of reproduced species over time in different C/O ratios and models.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: Abundance ratios of gas species relative to H in the MC2 and MC2_reacDes models.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: The fraction of reproduced species over time in different models.
Paper: Modeling Complex Organic Molecules’ Formation in Cold Cores: Multiphase Models with Nonthermal Mechanisms
Authors: Yang Lu, Donghui Quan, Qiang Chang, Long-Fei Chen, Di Li
Figure caption: Variation of D(t) over time across different models.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The corrections of extinction, colors, and brightness with MG0XPSP in the Giant I region. Panels (a)–(h) sequentially illustrate the correction of systematic biases based on extinction, color, brightness, and the simultaneous dependence of color and extinction using the LAMOST sample. Panels (i) and (j) show the correction for brightness-dependent systematic biases when G < 10, based on the PASTEL sample. The second row of panels presents the results after each correction step. Panels (k)–(r) show the final residuals on E(B − V), (BP − RP)0XPSP, G, MG0XPSP, [Fe/H]Spectra, [Fe/H]Gaia, and the H-R diagram, respectively. The yellow solid lines in panels (a), (c), (e), and (i) represent the corrections. In panels (g), (h), and (r), the colors of the dots indicate Δ[Fe/H], as coded on the color bar to the right. The red dots in panels (o), (p), and (q) are sources from the PASTEL sample, while the background dots are sources from the LAMOST sample.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The color–color diagrams of (BP − RP)0XPSP versus (BP − G)0XPSP, along with the H-R diagrams of sources in the Giant II region. The left column represents the sources from LAMOST, while the middle column represents the sources from PASTEL. The colors of the points indicate the [Fe/H] values, coded by the color bars. The term Δ (BP − G)0XPSP represents the residuals derived from the quadratic function fitting of (BP − RP)0XPSP to (BP − G)0XPSP, aiming to characterize the sensitivity of (BP − G)0XPSP to [Fe/H]. The upper right panel illustrates the relationship between the relative distance errors and distance, with the red solid line employed to exclude sources with significant relative distance errors. The lower right panel depicts the relationship between [Fe/H] and MG0XPSP after excluding these sources.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Stellar loci fitting residuals. From top to bottom, we show the Dwarf region, the Giant I region without and with MG0XPSP, and the RC–HB region, respectively. The first, second, and third columns show the residuals, as functions of ﹩{(B{P}_{\mathrm{XPSP}}-R{P}_{\mathrm{XPSP}})}_{0}﹩, [Fe/H]Spectra, and MG0XPSP, respectively, with the red points indicating PASTEL sources. The fourth column illustrates the distributions of residuals, with the red bar employed to compute the standard deviation of the Gaussian distribution, mitigating the impact of a limited number of outliers. The fifth column displays the distributions of residuals in the H-R diagram, where the colors of the points correspond to the residuals, as coded on the color bar to the right.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The H-R diagrams of the Giant I and RC–HB regions in different [Fe/H] ranges. The colors of the dots indicate the differences in [Fe/H] between this work and LAMOST (small dots) as well as PASTEL (large dots), as coded on the color bar to the right. The solid green lines in the upper left two panels distinguish the regions of red stragglers or subgiants.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The same as Figure 8 but showing the results of the corrections. The colors of the dots indicate the differences in [Fe/H] between this work and LAMOST (small dots) as well as PASTEL (large dots), as coded on the color bar to the right.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: The same as Figure 8 but for the Dwarf region. The solid green curves distinguish the regions of likely main-sequence binaries. The green vertical solid lines distinguish the regions of likely blue stragglers. The colors of the dots indicate the differences in [Fe/H] between this work and LAMOST (small dots) as well as PASTEL (large dots), as coded on the color bar to the right.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Distributions of the reference sample in ﹩{(B{P}_{\mathrm{XPSP}}-R{P}_{\mathrm{XPSP}})}_{0}﹩ versus ﹩{(B{P}_{\mathrm{XPSP}}-{G}_{\mathrm{XPSP}})}_{0}-({f}_{2}+{f}_{3})/1000﹩, color coded by [Fe/H], as shown by the color bar to the right. The lines from top to bottom represent our best fits of f1/1000 for [Fe/H] values of  +0.5, 0.0, −0.5, −1.0, −1.5, −2.0, −2.5, −3.0, −3.5, and  −4.0, respectively.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Similar to Figure 2, but for the comparisons between [Fe/H]Gaia and [Fe/H]Spectra of the reference sample, where the colors of the points correspond to the residuals, as coded on the color bar to the right.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Fitting residuals in the Giant II region.
Paper: Stellar Loci. VIII. Photometric Metallicities for 100 Million Stars Based on Synthetic Gaia Colors
Authors: Bowen Huang, 博闻 黄, Haibo Yuan, 海波 苑, Shuai Xu, 帅 徐, Kai Xiao, 凯 肖, Maosheng Xiang, 茂盛 向, Yang Huang, 样 黄, Timothy C. Beers
Figure caption: Test results for star clusters. The title of each column sequentially lists the name of the cluster, number of member stars, Galactic latitude, extinction, and distance. The first row of panels displays the metallicity distribution for member stars of each cluster. Their standard deviations after multiple 3 − σ clipping are labeled above each column. The median [Fe/H] of the member stars in each cluster, as derived from APOGEE DR17, is indicated by the green vertical lines. The second row of panels depicts the distribution of [Fe/H]Gaia from our results, along with MG0XPSP and G, represented by the left and right vertical coordinates, respectively. The third row of panels shows the H-R diagrams of these clusters, with the colors of the dots denoting [Fe/H]Gaia, as coded on the color bar on the right. The vertical coordinates are the same as those in the second row.