adsabs/AstroCLIMB huggingface dataset:
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Sky coverage of the NSS40 and NSS80 surveys as a function of flux sensitivity, for the hard (8−24 keV) energy band. The green and blue solid lines show the area curves for the overall NSS40 and NSS80 surveys, respectively. We compare with the other completed components of the NuSTAR extragalactic surveys program, which include the following dedicated deep-field surveys: COSMOS (dashed–dotted black line), ECDFS, EGS, GOODS-N, and UDS. The total area for these deep-field surveys is shown as a black solid line. We also compare to Cycle 5 of the NuSTAR extragalactic survey of the JWST north ecliptic pole (NEP) time-domain field, shown as a dotted black line (Zhao et al. 2021b).
Paper: LADDER: Revisiting the Cosmic Distance Ladder with Deep Learning Approaches and Exploring Its Applications
Authors: Rahul Shah, Soumadeep Saha, Purba Mukherjee, Utpal Garain, Supratik Pal
Figure caption: Results of ablation studies and validation experiments with various models. (i)–(iii) Variation of error, smoothness, and monotonicity with K, respectively. MLP models do not produce smooth, monotonic results (except K = 1), and the K = 1 MLP is outperformed by the LSTM model at roughly the same smoothness and monotonicity. (iv) Prediction variation of models trained on Σ∣λ and Σ0. When the covariance matrix is progressively corrupted with noise, the predictions change, thus demonstrating our approach’s ability to model correlations.
Paper: LADDER: Revisiting the Cosmic Distance Ladder with Deep Learning Approaches and Exploring Its Applications
Authors: Rahul Shah, Soumadeep Saha, Purba Mukherjee, Utpal Garain, Supratik Pal
Figure caption: Schematic overview of the training algorithm.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: The distributions of R  λ8542 and ﹩{R}_{\lambda 8542}^{+}﹩ with stellar parameters. From left to right are T eff, [Fe/H], and ﹩\mathrm{log}\ g﹩. The upper section in each panel is for the R index and the lower is for R +, as indicated in the plots. The red dashed line in the lower left panel is the lower 2σ line to selected inactive stars in Figure 8. Star symbols are bright stars with well-studied activity in Baliunas et al. (1995) and Hall et al. (2007, 2009). Spectra are extracted from the ESO archive. Inactive stars: HD 1461, HD 3795, HD 9562, HD 45067, HD 126053, HD 187691, HD 197076. Moderately active stars: HD 16160, HD 16673, HD 20630, HD 30495, HD 35296, HD 39587, HD 88873, HD 155885, HD 160346. Highly active stars: HD 17925, HD 22049. See text for details.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: The top and middle panels show the proportion of highly active and inactive stars, respectively. The bottom panel shows the number count of different categories in different temperature bins, as indicated by the different colors.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Linear regression is performed for each pair of R + values, with the corresponding residuals between the data and the fitted line shown in the lower panels. The left column displays ﹩{R}_{\lambda 8498}^{+}﹩– ﹩{R}_{\lambda 8542}^{+}﹩, the middle column shows ﹩{R}_{\lambda 8498}^{+}﹩–﹩{R}_{\lambda 8662}^{+}﹩, and the right column depicts ﹩{R}_{\lambda 8542}^{+}﹩–﹩{R}_{\lambda 8662}^{+}﹩. The red dashed lines represent the regression equations obtained from fitting the data, while ρ corresponds to the Pearson correlation coefficient.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: High-resolution spectrum of HD 22049. Top left: Ca II K; top right: Ca II H; bottom: Ca II λ8542.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Distribution of uncertainties for the spectral lines λ8498, λ8542, and λ8662 in three columns from left to right. Each column includes two panels, with the top one showing the distribution of uncertainty for R and its individual component, and the bottom one displaying the distribution of uncertainty for R +, both represented by the red histograms.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Comparison of different normalization methods in IRT bandpass. The upper panel is the emission-line spectrum and the lower is the absorption-line spectrum. The blue curve is the local normalized spectra from this work and the black curve is the global normalized spectra provided by LAMOST DR9.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Difference of two interpolation methods. Black dots are the observed spectrum; the blue curve is the cubic spline interpolation of the spectrum; the orange-dashed curve is the linear interpolation; the red dotted–dashed line shows the vacuum wavelength of λ8542.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Comparison of R index derived from 1 Å to 2 Å widths, respectively, for each IRT line. Red dashed lines are obtained by least-squares fitting of the data.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption:                       ﹩{R}_{\lambda 8542}^{+}﹩ vs. S index distribution. The background gray points are the same as Figure 10. The overlaid color samples are stars crossmatched with Gaia DR3 eclipsing binaries and RS-CVn variables. As indicated in the plot, these two samples coincide with Branch 1 and Branch 2, as defined in Figure 11. The black-dashed line is the linear regression of the eclipsing binary sample, with the function given. Star symbols are the same as in Figure 6.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: (a) Distribution of S−﹩{R}_{\lambda 8542}^{+}﹩; different branches are defined by eye and plotted in different colors, as indicated in the frame. The background stars are shown in gray. (b) Distribution of Branch 1 stars in stellar parameter space. Metallicity is indicated by color, as shown in the bottom color bar. (c) Distribution of Branch 2 stars. (d) Distribution of Branch 3 stars.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Typical spectra from the three branch stars are shown in Figure 11. The panels from top to bottom show a star of Branches 1, 2, and 3 respectively. The spectra and the corresponding templates of the Ca II IRT region and the Ca II H and K region are plotted.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: The top-left panel shows the relationship between the S index and R  λ8542, while the bottom-left panel illustrates the relationship of the S index and ﹩{R}_{\lambda 8542}^{+}﹩. The colors of each point represent their temperature, as indicated by the color bar. To make a clear view of how the indices' distributions change with the temperature, the small panels on the right-hand side show a similar distribution of indices as the left panels, but with the T eff range limited to 200 K.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Left panel: relationship of ﹩{R}_{\lambda 8542}^{+}﹩ vs. ﹩\mathrm{log}{R}_{\mathrm{HK}}^{+}﹩. Right panel: relationship of R  λ8542 vs. ﹩\mathrm{log}{R}_{\mathrm{HK}}^{+}﹩. Red and yellow points represent stars from Branch 1 and 2 as defined in Figure 11.
Paper: The Near-infrared Ca II Triplet as a Stellar Activity Indicator: A Library and Comparative Study
Authors: Xin Huang, 鑫 黄, Yuji He, 玉吉 何, Zhongrui Bai, 仲瑞 白, Hailong Yuan, 海龙 袁, Mingkuan Yang, 明宽 杨, Ming Zhou, 明 周, Yiqiao Dong, 义乔 董, Mengxin Wang, 梦欣 汪, Han He, 晗 贺, Jinghua Zhang, 敬华 张, Yaoquan Chu, 耀泉 褚, Yongheng Zhao, 永恒 赵, Yong Zhang, 勇 张, Haotong Zhang, 昊彤 张
Figure caption: Distribution of inactive, normal, and highly active stars in the T eff and log g space. Different colors represent different [Fe/H], as indicated by the color bar.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Spectra of neutrino opacities for ν  l  (﹩{\bar{\nu }}_{l}﹩) absorption on neutrons (protons), inverse β decay, and ν N elastic scattering under various approaches, with and without different modifications, at a thermodynamic point in the hot ring region near the core of a BNS postmerger (point (III) in Table 3). The opacities of absorption by nucleons, inverse β decay, and elastic scattering are represented by red, blue, and green, respectively, while various line styles are used to represent the opacities with or without corrections and different treatments of calculations. The abbreviations WM, PS, FF, MM, Elastic, Rec, and Strange correspond to weak magnetism, pseudoscalar, form factor, medium modifications, elastic approximation, approximated recoil, and strange-quark contributions, respectively. The opacities of ν  l  (﹩{\bar{\nu }}_{l}﹩) absorption by nucleons, calculated using the full kinematics approach and incorporating all available corrections, are 2–3 orders of magnitude higher than those computed using the elastic approximation with approximated corrections from Horowitz (2002). The opacity of inverse β decay is activated due to the medium modifications. The opacity of inverse β decay with elastic approximation and without medium modifications is completely suppressed in the given comparison.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Spectra of neutrino opacities defined in Equation (71) as a function of neutrino energy ε of the weak interactions included in Weakhub at thermodynamic point (I) in Table 3, which corresponds to the central region of s15s7b2 in Woosley & Weaver (1995). Note that the absorption opacities are computed using the full kinematics approach and all available corrections, and the scattering opacities incorporate all of the corrections as mentioned. Absorption processes, elastic scattering, inelastic scattering, and pair processes are represented by red, green, orange, and blue, respectively. We rescale opacities by multiplying 108 for ν e + inelastic scattering, 1010 for e − e + annihilation, 1015 for N–N bremsstrahlung, 107 for the plasma process, and 106 for the nuclear de-excitation process, respectively.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Comparison of the radial profiles of several quantities against the isotropic radial coordinate r between Weakhub (Con) and NuLib at the moment of core bounce of a 15 M ⊙ star. The dashed lines and solid lines correspond to the results obtained by Gmunu with NuLib and Weakhub (Con) (Weakhub with a conventional set of interactions), respectively. The profiles include rest mass density ρ, radial velocity v  r /c, matter temperature T, entropy per baryon s, neutrino rms energy observed in the fluid comoving frame ﹩\sqrt{\langle {\epsilon }_{{\nu }_{l}}^{2}\rangle }﹩, and electron fraction Y  e . The results obtained by using Weakhub (Con) quantitatively agree with the results obtained using NuLib.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Same as Figure 1 but at thermodynamic point (III) in Table 3, which corresponds to the hot ring region near the core of a hypermassive neutron star remnant formed from a BNS merger system, with consideration of a tiny muon fraction. Here, the opacities are without rescaling.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Comparison of the radial profiles of several quantities against the isotropic radial coordinate r at the moment of core bounce of a collapsing 20 M ⊙ star, with three sets of interactions in Weakhub. The dashed–dotted lines, dashed lines, and solid lines correspond to the results with interactions of conventional set (Con), advanced set (I) (Adv.I), and advanced set (II) (Adv.II), respectively. The profiles include rest mass density ρ, matter temperature T, electron fraction Y  e , and neutrino rms energy observed in the fluid comoving frame ﹩\sqrt{\langle {\epsilon }_{{\nu }_{l}}^{2}\rangle }﹩. All results quantitatively agree well with discrepancies of less than 5%, except for the approximately 28% and 40% higher values of ﹩\sqrt{\langle {\epsilon }_{{\bar{\nu }}_{e}}^{2}\rangle }﹩ and ﹩\sqrt{\langle {\epsilon }_{{\nu }_{x}}^{2}\rangle }﹩, respectively, outside the shocked region for the case of Adv.II.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Same as Figure 1 but at thermodynamic point (II) in Table 3, which corresponds to the central region of a hot PNS after core bounce with a tiny fraction of muon fraction, where the neutrino trapping and thermalization of ν  μ  and ν  τ  occur. Here, the opacities are without rescaling.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Time evolution of far-field neutrino rms energies ﹩\sqrt{\langle {{\epsilon }_{{\nu }_{l}}}^{2}\rangle }﹩ (left panel) and luminosities ﹩{L}_{{\nu }_{l}}^{\mathrm{fluid}}﹩ (right panel) measured by an observer comoving with the fluid at 500 km of a collapsing 15 M ⊙ star. The solid lines and dashed lines represent the results obtained by Weakhub (Con) (Weakhub with a conventional set of interactions) and NuLib, respectively. The results obtained using Weakhub (Con) agree well with those using NuLib, with discrepancies of less than ∼10% in rms energies and luminosities for all neutrino species.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Time evolution of far-field neutrino luminosities, ﹩{L}_{{\nu }_{l}}^{\mathrm{Euler}}﹩, observed by an Eulerian observer at a distance of 500 km from a collapsing 20 M ⊙ star. Dashed lines and solid lines correspond to the results with the advanced set (I) and (II) interactions (i.e., Adv.I and Adv.II), respectively. Dashed–dotted lines, loosely dotted lines, and dotted lines correspond to the results of Adv.II with cutoff density values for ﹩{\nu }_{e}{\bar{\nu }}_{e}﹩ pair annihilation of ρ cut = 1011 g cm−3, ρ cut = 1012.5 g cm−3, and ρ cut = 0 without the conservation treatment in Equation (70), respectively.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Time evolution of far-field neutrino rms energies observed in the fluid comoving frame ﹩\sqrt{\langle {{\epsilon }_{{\nu }_{l}}}^{2}\rangle }﹩ (left panel) and luminosities ﹩{L}_{{\nu }_{l}}^{\mathrm{Euler}}﹩ (right panel) measured by an Eulerian observer at 500 km of a collapsing 20 M ⊙ star. The dashed–dotted lines, dashed lines, and solid lines correspond to the results of Con, Adv.I, and Adv.II, respectively. The neutrino luminosities and rms energy values in Adv.I and Adv.II show significant differences compared to Con. For instance, at a time of t − t bounce = 70 ms, the results of Adv.II have relative differences of ﹩\left[+5.7 \% ,+12.7 \% ,+7.8 \% \right]﹩ (﹩+7.9 \% ,+13.1 \% ,+47.8 \% ﹩) in the values of ﹩\sqrt{\langle {{\epsilon }_{{\nu }_{l}}}^{2}\rangle }﹩ (﹩{L}_{{\nu }_{l}}^{\mathrm{Euler}}﹩) for the neutrino species ﹩\left[{\nu }_{e},{\bar{\nu }}_{e},{\nu }_{x}\right]﹩ when compared to the results of Con.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub 
Authors: Harry Ho-Yin Ng, Patrick Chi-Kit Cheong, 志杰 張, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Time evolution of the radius of PNS (dashed lines), which is defined as the radius for ρ > 1011 g cm−3 and the shock radius (solid lines), which is defined as the radius from the center to the position where the velocity is minimum. Lines with blue, red, and black colors represent the radii of the simulations of Con, Adv.I, and Adv.II, respectively. Results of Adv.II exhibit the shortest shock radius and PNS radius, primarily because of the rapid cooling of external ν  x  emissions through ﹩{\nu }_{e}{\bar{\nu }}_{e}﹩ pair annihilation and the kernel forms of other pair processes.
Paper: Statistical Analyses of Solar Prominences and Active Region Features in 304 Å Filtergrams Detected via Deep Learning
Authors: T. Zhang, Q. Hao, P. F. Chen
Figure caption: An observed 304 Å image obtained on 2014 June 1 as an example to show the detection modules. (a) The raw data after a logarithmic rescaling. (b) The predicted prominence and AR candidates directly from U-Net are marked as green “+” and red “×,” respectively. (c) The final prominences and ARs after the postprocessing. The symbols have the same mean as (b). (d)–(f) The ring-shaped off-limb regions are transformed into rectangles in polar coordinates with different rescaling methods. (g) The manually labeled prominences (green), ARs (red), and background (blue). (h) The predicted prominence and AR candidates by our U-Net model. (i) The final detected results after the postprocessing. The yellow blocks stand for the intersection between prominences and ARs. Panels (j)–(l) are the enlarged parts of (f), (h), and (i), giving the zoomed-in details.