adsabs/AstroCLIMB huggingface dataset:
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Initial estimates (a) and clustering results (b) for 25 spatially adjacent H I spectra. In both panels, black solid lines represent the observed spectra. In (a), red dots and bars denote the estimated Gaussians, where the x-coordinate of a red dot corresponds to the line-center, the y-coordinate represents half of the peak intensity, and the bar width indicates the FWHM. Green solid lines show the total intensity of these Gaussians. In (b), colored lines depict the multi-Gaussian fitting results, with lines of the same color and style indicating Gaussians grouped into the same structure. The black dashed line represents the total intensity of all Gaussians. The numbers in the top-left parentheses of each LoS indicate the (α,  δ) coordinate values, while the middle-left numbers denote the angular separation from the central LoS.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: (a) Integrated intensity map of HI4PI data, (b) distribution of the number of Gaussians in equatorial coordinates, and (c) histogram of central velocities of Gaussians. The color scales in (a) and (b) represent the integrated intensity and the number of Gaussians, respectively.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The (a) line-center velocity, (b) FWHM line width, and (c) peak intensity map of one H I structure in the HI4PI all-sky decomposition result.
Paper: Highly Polarized Intrinsic Emission and Its Orthogonal Counterpart in Vela X-1
Authors: WanYun Wu, Fei Xie, Long Ji, MingYu Ge, Fabio La Monaca
Figure caption: Corner plot of the posterior distribution for the parameters of RVM fitted to phase-resolved PA1, as discussed in Section 3.3. The range of ip is confined to 73°–107°. The two-dimensional contours correspond to 68.3%, 95.45%, and 99.73% confidence levels. The histograms show the normalized one-dimensional distributions for a given parameter derived from the posterior samples.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Density map of Gaussian fit parameters (Tpeak, FWHM) for all HI4PI components, where darker regions indicate higher densities in parameter space. The top and right panels display the marginal histograms of Tpeak and FWHM, respectively.
Paper: Highly Polarized Intrinsic Emission and Its Orthogonal Counterpart in Vela X-1
Authors: WanYun Wu, Fei Xie, Long Ji, MingYu Ge, Fabio La Monaca
Figure caption: Same as Figure A1, but for the simultaneous fit to phase-resolved PA1 and PA2,3.
Paper: Highly Polarized Intrinsic Emission and Its Orthogonal Counterpart in Vela X-1
Authors: WanYun Wu, Fei Xie, Long Ji, MingYu Ge, Fabio La Monaca
Figure caption: Same as Figure A1, but for phase-resolved PA2,3.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Face-on view of 12CO structures with an angular size larger than ﹩30\,{{\rm{arcmin}}}^{2}﹩. Circles represent the structures, with their radii indicating relative sizes and the color representing the densities of structures in space. The Sun is located at (0, 0) kpc, and the Galactic center is at (8.15, 0) kpc. The first and third plots show subregions of the second one, as indicated by the gray dashed lines and boxes, while the fourth plot is a subregion of the third one. Blue, black, purple, and red solid lines trace the centers of the Local, Perseus, Norma-Outer, and Outer Scutum–Centaurus Arms, respectively, with dashed lines indicating their widths (M. J. Reid et al. 2019).
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Histogram of (a) angular area, (b) velocity span, and (c) total flux of GDCluster (blue) and DBSCAN (red) structures.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Density map of mean peak intensity vs. FWHM for all HI4PI H I structures. Each point represents an individual structure, with the blue indicating denser regions in parameter space. The top and right panels display the marginal histograms of mean peak intensities and FWHM, respectively.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 4 for 12CO Gaussians. The blue dashed line denotes the bound of two distinct clusters.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 5 for a 12CO structure. In panel (d), the wider (W) type of Gaussians in Figure 11 are displayed in yellow, while the narrower (N) types are displayed in blue.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 2 for 12CO data.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 2 for CRAFTS H I data in a 10° × 10° subregion.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 6 for CRAFTS H I structures.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 4 for CRAFTS H I Gaussians.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Simulated spectra and decomposition results for Δv =  (a) 3σv, (b) 4σv, (c) 5σv. Line styles match Figure 18; the magenta line illustrates the additional DBSCAN structure.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Spectra and decomposition results for several adjacent LoSs. Gray solid lines: observed spectra; cyan solid line: single DBSCAN structure; black solid line: Gaussian components decomposed by GaussPy+; dashed lines: four different GDCluster structures distinguished by different colors.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Histogram of (a) GDCluster structures covered by one DBSCAN structure and (b) DBSCAN structures covered by one GDCluster structure. The gray dashed line in panel (b) separates the x-axis into linear- and logarithmic-scale regions.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Simulated spectra and decomposition results for nine sightlines. Gray: simulated; blue/green dashed: GDCluster components; cyan: single DBSCAN structure.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: Density map of the flux of DBSCAN and GDCluster structures. Red indicates denser regions; the black dashed line marks the 1:1 flux relationship.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 2 for C18O data. The intensity is integrated over the entire velocity range, resulting in a noise-like moment 0 map.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 4 for all (a) 13CO and (b) C18O Gaussians.
Paper: Atomic and Molecular Gas in the Milky Way. I. Structure Decomposition
Authors: Xin Liu, Fujun Du
Figure caption: The same as Figure 2 for 13CO data.
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: The impact of IMF clock angle on ion mixing rates. The calculation of mixing rates and the statistics of particle flux are analogous to Figure 2. The perspective of these diagrams is from the Sun looking toward the Earth, with the horizontal axis representing the dawn–dusk direction and the vertical axis indicating geomagnetic north–south poles. Black clocks with red arrows indicate the corresponding IMF clock angle conditions for each case.
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: The influence of solar wind dynamic pressure on ion mixing rates under the same northward IMF condition. The mixing rates are represented in the equatorial plane, where KH fluctuations are believed to be most intense. From left to right, panels (a)–(e) demonstrate the trend in mixing rates at the magnetopause boundary layer under conditions corresponding to increasing dynamic pressures (P from <0.5 nPa to >10 nPa).
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: Quantitative statistical results for the fluxes of entering solar wind ions (a) and escaping magnetospheric ions (b) traversing the magnetopause under different solar wind dynamic pressure conditions. The illustration features five concentric circles, each representing a distinct scenario, arranged from the innermost to the outermost layers, with increasing dynamic pressures ranging from <0.5 nPa to >10 nPa, as indicated by red arrows. For each concentric circle, average flux measurements in six magnetopause sectors defined by north–south and dawn–dusk orientations are annotated within their respective sectors.
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: Quantitative statistical results of the fluxes of entering solar wind ions (a) and escaping magnetospheric ions (b) traversing the magnetopause under different IMF clock angle conditions. In panels (a) and (b), eight colored circles represent eight different clock angle cases. The directions of the clock angles are indicated by red arrows on the adjacent black clocks, respectively. For each case, the magnetopause is divided into six sectors, as illustrated in Figure 4, to quantify and annotate the fluxes in each region.
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: The corresponding influence of solar wind dynamic pressure on the fluxes of entering solar wind ions (blue) and escaping magnetospheric ions (red) is shown on the magnetopause. The 3D magnetopause surface is obtained from the peaks in mixing rates as depicted in Figure 2.
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: Corresponding fluxes of entering solar wind ions and escaping magnetospheric ions across the magnetopause under different IMF clock angle conditions.
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: Magnetopause Kelvin–Helmholtz waves under a northward IMF condition. (a) The magnetic field B (nT), (b) the ion bulk velocity Vx (km s−1), and (c) and (d) the number densities of solar wind ions Nsw (cm−3) and magnetospheric ions Nmp (cm−3), respectively.
Paper: Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
Authors: Zhongwei Yang, Can Huang, Xiaocheng Guo, Riku Jarvinen, Binbin Tang, Wence Jiang, Hui Li, Chi Wang
Figure caption: The time evolution of the fluxes, averaged from the dawn and dusk sectors at low latitudes, for solar wind particle injection (solid) and planetary particle loss (dashed), respectively. The curves, ranging from thin to thick, correspond to results from runs 1–5 under varying solar wind dynamic pressure conditions (denoted on the right side of the figure).
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: Photometry results. Left: the g mag error distribution. Orange dots represent the mean errors in g mag bins with error bars representing the standard deviations. The vertical line marks the completeness limit of g = 23.5, where the mean error is around 0.03 mag, marked by the horizontal line. Middle: the completeness as a function of g mag. The error bars represent Poisson uncertainties based on the number of artificial point sources injected for the completeness test. The completeness limit of g = 23.5 is indicated by the vertical dashed line, while the horizontal line represents the completeness of 92.5%. Right: the radial completeness function for sources with 22 < g < 23. The error bars represent Poisson uncertainties, and the orange curve is the exponential function fitted to the completeness in radial bins.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: Distributions of excess factors. Left: AEN against g mag for stars (blue shading), galaxies (orange dots), and GCs (green triangles). The red solid curve represents the threshold for GC selecting candidates. Middle: similar to the left but for BRexcess. The red dashed horizontal line represents the criterion of BRexcess =2.5 for excluding galaxies. Right: the cumulative BRexcess distributions of stars (blue), galaxies (orange), and GCs (green).
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The g-band images of NGC 3115. Left: the central region of the original g-band image. Middle: the elliptical model. Right: the residual image after subtracting the model.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The radial variation in g-band GCLF. Panel (a) displays GCLFs in various radial bins. The color scheme is such that lighter colors correspond to larger radii. The vertical lines indicate the turnover magnitude for different radial bins. Panel (b) and panel (c) show the radial variations of turnover magnitude (Mg,TO) and dispersion (σg), respectively. The horizontal error bars represent the radial ranges for corresponding bins, and vertical error bars represent the 16th and 84th percentiles of the MCMC samplings. The red dashed line and curve represent the best-fit relations for Mg,TO and σg, respectively.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: Projected density maps of GC candidates showing substructures. The maps are shown at two different scales, ﹩35^{\prime} ﹩ (top) and ﹩70^{\prime} ﹩ (bottom), and for three GC subsamples, all candidates (left), red candidates (middle), and blue candidates (right). These distributions are measured using Gaussian kernel density estimation (KDE), with the kernel sizes indicated by the small black circles in the lower right corners of each panel. The contours represent 1σ (gray), 2σ (blue), 3σ (green), and 5σ (orange) above the mean background density, which is estimated within the shaded annular regions. The green ellipses in the top panels represent the isophote of ﹩{\mu }_{g}=25\,\mathrm{mag}\,{\mathrm{arcsec}}^{-2}﹩ measured on g-band image. The center of NGC 3115 and 3115B are indicated as a red plus symbol and a red cross, respectively. The NE excess, N clump, and E clump are marked by the red star, a red triangle, and a red inverted triangle, respectively.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The g-band GCLF of the entire GCS. The open and hatched histograms show the raw distribution of GC candidates (without background subtraction) within 70′ and the central 30′, respectively. The black dots with error bars, representing the background-subtracted GC number in the same g mag bins as in Section 3.1, are used for fitting the Gaussian GCLF. The light red curves represent Gaussian fittings for 200 random MCMC sampling of the measurements, illustrating the fitting uncertainty. The fitted GCLF parameters, total number of genuine GCs, and the corresponding specific frequency of GCs in NGC 3115 are given in the upper left corner. The best-fit turnover magnitude is also indicated as the dashed vertical line. See Section 3.2.1 for more details.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: GC color distributions. The leftmost column shows the normalized color distributions of contaminants, with blue solid curves constructed using Gaussian KDE. The contaminant sample is defined as candidates located between ﹩40^{\prime} ﹩ and ﹩70^{\prime} ﹩. The remaining columns show the normalized raw (dashed) and background-corrected (solid) color distributions in six radial bins, with radial ranges indicated in the panel titles. These curves represent probability density functions (PDFs), normalized such that the total area under each curve is unity. The blue dashed–dotted curves and shaded regions represent the expected background distribution scaled by the corresponding contaminant fractions, which are subtracted from the raw distributions to obtain the background-corrected ones.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The morphological parameters. The cumulative distributions of ELLIPTICITY, FWHM, and CLASS_STAR are shown in the left, middle, and right columns, respectively. The results for the g, r, and z band are displayed in the top, middle, and bottom rows, respectively. The red dashed vertical lines in each panel represent the criteria for selecting GC candidates, and the blue- and orange-shaded regions represent the excluded ranges for stars and galaxies, respectively.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The radial color variations of GC candidates. The g − z and g − r colors are shown in the left and right panels, respectively. The little dots are individual GC candidates, plotted according to the g − z and g − r colors. The large dots represent contaminant-corrected peak colors of the GC distributions at different radii, with horizontal error bars representing the radial range and vertical error bars obtained from bootstrapping 100 times. The best-fit linear dependence of peak colors on ﹩\mathrm{log}R﹩ are shown as solid curves. See Section 3.3 for details.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: Sérsic profile parameters as functions of g mag. Panel (a) shows the Sérsic index n, panel (b) shows the surface density at the effective radius Σe, and panel (c) shows the effective radius of the GC system normalized by the stellar effective radius, Re,gc/Re,⋆. Vertical error bars represent the 16th and 84th percentiles of the MCMC sampling, while horizontal error bars indicate the magnitude range of each bin. Red dashed lines in panel (a) and (c) indicate the best-fit linear trends in n and Re,gc/Re,⋆, respectively.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The g − r vs. r − z diagram. The left panel presents all sources as the gray shading. The distributions of stars and galaxies are represented, respectively, as blue and orange contours. Individual fiducial GCs are indicated as green triangles. The middle and right show the remaining non-Gaia and Gaia sources after previous selection, respectively. The red ellipse represents the GC region.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The Sérsic radial density profiles of the entire (black), the brightest (orange), and the faintest (blue) GC candidate samples. The data points are only for visual inspection, with error bars representing Poisson errors. The vertical and horizontal lines indicate the effective radii and the background levels, respectively. The light-colored curves show 200 random MCMC samplings that illustrate the fitting uncertainties. The gray shading indicates the region between ﹩40^{\prime} ﹩ and ﹩70^{\prime} ﹩ used for background estimation.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Top left: F275W, F275W − F336W CMD of the internal field zoomed in around the MSTO region for all sources with an error in magnitude of F275W and magnitude of F336W < 1. A BaSTI α-enhanced isochrone for t = 12 Gyr, Z = 0.002, and Y = 0.248, is overplotted as a solid light blue line. The model was transformed to the observed plane by using the reddening and extinction values listed in Section 3.1. The theoretical MSTO at M = 0.8 M⊙ is marked with a golden star. The thicker section of the isochrone indicates a mass width ﹩\delta { \mathcal M }=\pm 0.004﹩ around 0.8 M⊙ of 20.88 ≤ F275W ≤ 21.03. Stars selected in this MSTO region are marked as green dots. Top right: color histogram of the MSTO selected stars. The dotted blue vertical lines mark the ±1.5σ color cut used to select the final sample of MSTO stars. Bottom left: final sample of MSTO stars in the same CMD. The F275W magnitude bin is split in half, with the stars in the upper (N = 1970) and bottom bin (N = 1902) marked with pink and purple dots, respectively. Stars discarded by the color selection are marked with green dots. Bottom right: a BaSTI evolutionary track for M = 0.8 M⊙ (solid orange line) and the same isochrone (solid light blue) are overplotted on the MSTO region of the CMD. The filled black circles on the track mark the F275W magnitudes used to calculate the MSTO crossing times (see Table 2 for more details).