adsabs/AstroCLIMB huggingface dataset:
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: Sample of response curves and detection thresholds for EPR (Equation (7)), PC (Equation (6), and DCC (Equation (5)). (Top left) Poisson background with λ = 5 and a chirp-like signal injected to the two channels. EPR is applied with κ = 0.5 in Equation (1). For EPR, two response curves are shown following a split of real-valued data into positive (“P”) and negative (“N”) branches for conversion to Boolean data, together with their time-randomized versions. (Top right) The near-Gaussian case of Poisson λ  = 10,000 with otherwise the same chirp signal. (Bottom left) Background noise and signal are now drawn from uniform and Gaussian distributions, respectively, preserving the same κ as in the upper panels. (Bottom right) The same for Gaussian and sine wave as the background and signal, respectively.
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: (Left) PDF of EPR for background noise without signal injection. For random numbers (white noise), EPR has the expectation value 1 (blue curve). The same outcome is produced following time randomization (gray dotted line). (Right) With signal injection, the expectation value of EPR shows a positive shift correlated to signal amplitude (blue curve), while time randomization preserves the baseline.
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: Detection thresholds as in Figure 8 now with κ = 1.6 for EPR. While κ may change the ranking of PC and EPR based on DTμ and DTσ, Figure 12 shows this is limited to a few specific cases.
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: EPR applied to a pair of uncorrelated random arrays drawn from Poisson distribution. (Left) ﹩\overline{{\rm{EPR}}}\,=\,1﹩ and its standard deviation σ decreases with array size N. (Right) The standard deviation ﹩\sigma \,\propto \,1/\sqrt{N}﹩ follows the canonical result of random walks.
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: Background (horizontal) and signal (vertical) combinations based on Section 4.1 with Poisson parameters λ = 10,000 and λs = 5 and signal strength (Equation (3)) α = 0.5.
Paper: Asteroid Types, Albedos, and Diameters Catalog from Gaia DR3: Intelligent Inversion Results via Multisource Information Fusion
Authors: Jiayi Ge, Xiaoming Zhang, Juan Li, Huijuan Wang, Dawei Xu, Xiaojun Jiang
Figure caption: Framework of this study.
Paper: Digitization of Astronomical Photographic Plates from China: Photometric Calibration of Single-exposure Plates and Release of Photometric Catalogs
Authors: Mingyang Ma, Haibo Yuan, Kai Xiao, Bowen Huang, Tao Wang, Yang Huang, Shiyin Shen, Zhengjun Shang, Yong Yu, Liangliang Wang, Meiting Yang, Jing Yang, Min Liu, Quanfeng Xu, Chenzhou Cui, Dongwei Fan, Zhenghong Tang, Jianhai Zhao
Figure caption: Images and light curves of a supergiant star (﹩0{0}^{{\rm{h}}}3{7}^{{\rm{m}}}20\mathop{.}\limits^{{\rm{s}}}64,\,4{0}^{\circ }{16}^{{\rm{{\prime} }}}37\mathop{.}\limits^{\unicode{x02033}}70﹩) from M31 and its reference star. The images has a field of view of approximately ﹩3\mathop{.}\limits{{\rm{^{\prime} }}}2\times 5\mathop{.}\limits{{\rm{^{\prime} }}}6﹩, with plate name, observational time, exposure time, and calibrated magnitudes labeled. In the light-curve panels, the blue, yellow, and red points have variable_flag values of 3, 4, and 5, respectively. The μ and σ values represent the mean and standard deviation of all calibrated magnitudes. The shaded regions cover the 3σ area. The yellow and white dashed lines represent the standard magnitudes and the mean values of calibrated magnitudes, respectively. The three red rectangles correspond to the three images above.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Left: the 12 base HEALPix pixels at k = 0 resolution dividing the full sky into equal-area regions. Right: an example of refining the n = 4 base pixel to k = 2, resulting in an 8 × 8 grid. The main and secondary diagonals correspond to a Galactic longitude and latitude of 0∘, spanning 90∘. The numbers in each cell represent the HEALPix pixel IDs (with nested ordering).
Paper: Digitization of Astronomical Photographic Plates from China: Photometric Calibration of Single-exposure Plates and Release of Photometric Catalogs
Authors: Mingyang Ma, Haibo Yuan, Kai Xiao, Bowen Huang, Tao Wang, Yang Huang, Shiyin Shen, Zhengjun Shang, Yong Yu, Liangliang Wang, Meiting Yang, Jing Yang, Min Liu, Quanfeng Xu, Chenzhou Cui, Dongwei Fan, Zhenghong Tang, Jianhai Zhao
Figure caption: Fraction of variable candidates in the H-R diagram. The panels from left to right correspond to variable sources of variable_flag ≥ 3, 4, 5, respectively.
Paper: Digitization of Astronomical Photographic Plates from China: Photometric Calibration of Single-exposure Plates and Release of Photometric Catalogs
Authors: Mingyang Ma, Haibo Yuan, Kai Xiao, Bowen Huang, Tao Wang, Yang Huang, Shiyin Shen, Zhengjun Shang, Yong Yu, Liangliang Wang, Meiting Yang, Jing Yang, Min Liu, Quanfeng Xu, Chenzhou Cui, Dongwei Fan, Zhenghong Tang, Jianhai Zhao
Figure caption: Same as Figure 4 but for the plate SH6401V64087001.
Paper: Digitization of Astronomical Photographic Plates from China: Photometric Calibration of Single-exposure Plates and Release of Photometric Catalogs
Authors: Mingyang Ma, Haibo Yuan, Kai Xiao, Bowen Huang, Tao Wang, Yang Huang, Shiyin Shen, Zhengjun Shang, Yong Yu, Liangliang Wang, Meiting Yang, Jing Yang, Min Liu, Quanfeng Xu, Chenzhou Cui, Dongwei Fan, Zhenghong Tang, Jianhai Zhao
Figure caption: Same as Figure 4 but for the plate YN8105175001.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Bin widths as a function of distance. Colors indicate the use of different parameters in different regions, as discussed in Section 3.2.
Paper: Digitization of Astronomical Photographic Plates from China: Photometric Calibration of Single-exposure Plates and Release of Photometric Catalogs
Authors: Mingyang Ma, Haibo Yuan, Kai Xiao, Bowen Huang, Tao Wang, Yang Huang, Shiyin Shen, Zhengjun Shang, Yong Yu, Liangliang Wang, Meiting Yang, Jing Yang, Min Liu, Quanfeng Xu, Chenzhou Cui, Dongwei Fan, Zhenghong Tang, Jianhai Zhao
Figure caption: Same as Figure 4 but for the plate BJ8404DA3924001.
Paper: Digitization of Astronomical Photographic Plates from China: Photometric Calibration of Single-exposure Plates and Release of Photometric Catalogs
Authors: Mingyang Ma, Haibo Yuan, Kai Xiao, Bowen Huang, Tao Wang, Yang Huang, Shiyin Shen, Zhengjun Shang, Yong Yu, Liangliang Wang, Meiting Yang, Jing Yang, Min Liu, Quanfeng Xu, Chenzhou Cui, Dongwei Fan, Zhenghong Tang, Jianhai Zhao
Figure caption: Same as Figure 4 but for the plate ZT8409SN3433001.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: This figure presents the clustering results for the region corresponding to HEALPix pixel index 7 in Figure 1, spanning Galactic longitudes from 225∘ to 315∘ and latitudes from −45∘ to +45∘. The four panels correspond to different distance intervals: 0–0.3, 0.3–1, 1–3.5, and 3.5–10 kpc. Molecular clouds identified in each bin are outlined accordingly. The Dendrograms parameters used in each distance interval are listed in Table 1. Distinct clouds along the line of sight are represented using different colors.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Histograms of key physical properties of the molecular clouds cataloged in this work. Top left: physical radius; top right: total mass; bottom left: surface mass density; bottom right: average dust density. Solid red lines represent the full sample, dashed gold lines denote Local Bubble clouds, and dashed blue lines correspond to non–Local Bubble clouds.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Example projections of a dendrogram-clustering result. Top: ﹩X^{\prime} ﹩–﹩Y^{\prime} ﹩ plane (sky view). Middle: ﹩X^{\prime} ﹩–﹩Z^{\prime} ﹩ plane. Bottom: ﹩Y^{\prime} ﹩–﹩Z^{\prime} ﹩ plane. Here, ﹩Z^{\prime} ﹩ represents the line-of-sight (distance) direction, and ﹩X^{\prime} ﹩–﹩Y^{\prime} ﹩ corresponds to the celestial sphere, as described in Section 3.1. The color scale represents the average dust density (i.e., extinction gradient in mag kpc−1). For each projection, the mean is calculated using pixels enclosed by the white-dashed rectangles, which are selected to minimize contamination from overlapping lines of sight.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Spatial distribution of molecular clouds not associated with the Local Bubble in the X–Y, X–Z, and Y–Z planes. The Sun is located at (X, Y, Z) = (8.12, 0.00, 0.02) kpc, and the Galactic center at the origin. In the X–Y panel, clouds are shown as hollow circles with radii scaled to twice their actual physical radii to enhance visibility. Background shading reflects average dust density from the W25 map. The X–Z and Y–Z panels show clouds as black dots over the corresponding vertical dust distribution.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Sky distribution of cataloged molecular clouds in Galactic coordinates. Circle sizes represent angular radii, and colors indicate distances from the Sun. The void outlined by the red dashed line corresponds to the “chimney” structure identified by T. J. O'Neill et al. (2024), interpreted as a vertical opening of the Local Bubble. The “tunnel” feature described in the same study is outlined by the black dashed line.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Left: spatial distribution of molecular clouds within 0.3 kpc of the Sun, projected onto the X–Y plane. The Sun is at the origin. The color scale shows the vertical coordinate Z in parsecs. Right: molecular clouds likely associated with the Local Bubble boundary, selected using the distance threshold described in the text. Colors again represent Z.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Comparison of physical properties of molecular clouds in this work (excluding Local Bubble clouds; red) with those from M.-A. Miville-Deschênes et al. (2017; purple), B. Q. Chen et al. (2020; blue), H. L. Guo et al. (2022; green), and Y.-H. Xie et al. (2024; orange). Top: physical radius; middle: total mass; bottom: surface mass density. All plots show normalized histograms for comparison.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Distribution of molecular clouds in Galactic coordinates. Left: Galactic longitude vs. distance from the Sun. Right: Galactic latitude vs. distance. In both panels, each circle represents a molecular cloud. The radius of the circle reflects the physical size of the cloud, while its opacity indicates the average dust density—denser clouds appear more opaque.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Same as Figure 4, but for the region spanning Galactic longitudes 90∘–180∘ and latitudes 0∘–90∘, corresponding to HEALPix pixel index 1 in Figure 4.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: This figure presents the clustering results for the region corresponding to HEALPix pixel index 0 in Figure 1, spanning Galactic longitudes from 0∘ to 90∘ and latitudes 0∘–90∘. The four panels correspond to different distance intervals: 0–0.3, 0.3–1, 1–3.5, and 3.5–10 kpc. Molecular clouds identified in each bin are outlined accordingly. The Dendrograms parameters used in each distance interval are listed in Table 1. Distinct clouds along the line of sight are represented using different colors.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Spatial distribution of cataloged molecular clouds in the Galactic X–Y plane. Each circle represents a molecular cloud, with radius proportional to its physical size and transparency indicating average dust density (a proxy for compactness). The Sun is at (X, Y) = (8.12, 0) kpc. Galactic longitudes are labeled for orientation. Solid and dashed curves represent spiral arm loci and their ±1σ widths based on M. J. Reid et al. (2019). Several large-scale cavities are outlined with black dashed lines, including the “Giant Oval Cavity” described by J. L. Vergely et al. (2022) and the “Carina cavity” described by B. Q. Chen et al. (2019a). The “Lower Sagittarius–Carina Spur” described by B. Q. Chen et al. (2020) is outlined in purple.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Mass–radius relation for molecular clouds in our catalog. Green circles: Local Bubble clouds; gold circles: non–Local Bubble clouds within 1 kpc; blue circles: clouds beyond 1 kpc. The black solid line shows the best-fit for the blue population. Data from previous studies are shown for comparison: M.-A. Miville-Deschênes et al. (2017; gray circles), B. Q. Chen et al. (2020; red X markers), H. L. Guo et al. (2022; orange squares), S. Cahlon et al. (2024; pink triangles), and Y.-H. Xie et al. (2024; purple stars).
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes −45∘ to 45∘ and latitudes −45∘ to 45∘, corresponding to HEALPix pixel index 4 in Figure 4. The low-resolution region near the upper center of each panel, corresponding to the Galactic center direction, arises from the adaptive angular binning scheme used in W25, which is based on local stellar density. In this area, heavy dust extinction reduces Gaia’s detection depth, resulting in lower stellar densities and consequently coarser angular resolution.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Histograms of cloud physical properties under different clustering-parameter configurations. From top to bottom, the four panels show results obtained by modifying a single parameter from the baseline values listed in Table 1: (1) setting all min_value values to 0.01 mag kpc−1; (2) setting all min_delta values to 0.1 mag kpc−1; (3) setting all min_delta values to 0.5 mag kpc−1; and (4) setting all min_npix values to 500.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 180∘–270∘ and latitudes 0∘–90∘, corresponding to HEALPix pixel index 2 in Figure 4. The low-resolution regions near the top of each panel arise from the adaptive spatial binning in W25, which is based on local stellar density. These areas correspond to sky regions with relatively sparse Gaia coverage, resulting in reduced angular resolution.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 135∘–225∘ and latitudes −45∘ to 45∘, corresponding to HEALPix pixel index 6 in Figure 4.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 45∘–135∘ and latitudes −45∘ to 45∘, corresponding to HEALPix pixel index 5 in Figure 4.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 270∘–360∘ and latitudes 0∘–90∘, corresponding to HEALPix pixel index 3 in Figure 4.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 0∘–90∘ and latitudes −90∘ to 0∘, corresponding to HEALPix pixel index 8 in Figure 4. The low-resolution regions near the bottom of each panel arise from the adaptive spatial binning in W25, which is based on local stellar density. These areas correspond to sky regions with relatively sparse Gaia coverage, resulting in reduced angular resolution.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 270∘–360∘ and latitudes −90∘ to 0∘, corresponding to HEALPix pixel index 11 in Figure 4.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 180∘–270∘ and latitudes −90∘ to 0∘, corresponding to HEALPix pixel index 10 in Figure 4.
Paper: A Comprehensive All-sky Catalog of 3345 Molecular Clouds from Three-dimensional Dust Extinction
Authors: Tao Wang, 涛 王, Haibo Yuan, 海波 苑, Bingqiu Chen, 丙秋 陈, Guangxing Li, 广兴 李, Bowen Huang, 博闻 黄, Helong Guo, 贺龙 郭, Ruoyi Zhang, 若羿 张
Figure caption: Similar to Figure A2 but for the region spanning Galactic longitudes 90∘–180∘ and latitudes −90∘ to 0∘, corresponding to HEALPix pixel index 9 in Figure 4.
Paper: Hemispheric Asymmetry of Relative Sunspot Numbers during Solar Cycles 17–25
Authors: Wenhua Wang, Linhua Deng, Zuo Jiang, Jinlei Li, Xinhua Zhao, Tingting Xu, Miao Wan, Jie Cao, Nanbin Xiang, Xuewen Tan, Wei Zhou, Weihong Zhou
Figure caption: The variation of the cumulative sum of monthly mean sunspot numbers in the northern and southern hemispheres during SC17–SC25. Each panel corresponds to one solar cycle. The orange dashed line represents the cumulative sunspot counts in the northern hemisphere, while the solid purple line indicates those in the southern hemisphere. The difference between the two lines reflects the hemispheric asymmetry in sunspot activity over each cycle.
Paper: Hemispheric Asymmetry of Relative Sunspot Numbers during Solar Cycles 17–25
Authors: Wenhua Wang, Linhua Deng, Zuo Jiang, Jinlei Li, Xinhua Zhao, Tingting Xu, Miao Wan, Jie Cao, Nanbin Xiang, Xuewen Tan, Wei Zhou, Weihong Zhou
Figure caption: Sliding-window Pearson correlation coefficients between SC23 and SC25 sunspot numbers in the northern (top panel) and southern (bottom panel) hemispheres, using a 12 month window. The x-axis denotes the central index of each window. Positive correlations indicate consistent trends between cycles.
Paper: Automatic 3D Reconstruction of Coronal Mass Ejections Based on Dual-viewpoint Observations and Machine Learning
Authors: Rongpei Lin, 荣沛 林, Yi Yang, 易 杨, Fang Shen, 芳 沈, Gilbert Pi, Yucong Li, 雨淙 李
Figure caption: The reconstruction of the GCS model given different choices of β, an example of the CME event occurring on 2016 April 4. Panels (a) and (b) show the reconstruction when there is no area penalty, which is in the β  =  0 scenario. Panels (c) and (d) show the reconstruction when the area penalty is large, which is in the β  =  1 scenario. The blue wire frame represents the GCS model.
Paper: Automatic 3D Reconstruction of Coronal Mass Ejections Based on Dual-viewpoint Observations and Machine Learning
Authors: Rongpei Lin, 荣沛 林, Yi Yang, 易 杨, Fang Shen, 芳 沈, Gilbert Pi, Yucong Li, 雨淙 李
Figure caption: Workflow of the region acquisition step. The feature map is obtained from the processed, running-difference coronagraph images. Then, we reduce the dimension of the feature map to get the colocalization map with the PCA algorithm. Otsu’s algorithm is then employed to get the binary mask of the CME region.
Paper: Automatic 3D Reconstruction of Coronal Mass Ejections Based on Dual-viewpoint Observations and Machine Learning
Authors: Rongpei Lin, 荣沛 林, Yi Yang, 易 杨, Fang Shen, 芳 沈, Gilbert Pi, Yucong Li, 雨淙 李
Figure caption: Schematics of the GCS model. Panel (a) shows a planar cut of the model, which is viewed face on. Panel (b) shows a cut of the model which is viewed edge on. This figure is based on the work of A. Thernisien (2011).