adsabs/AstroCLIMB huggingface dataset:
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A1612. A merger between two equal-mass subclusters with a radio relic that is misaligned with the WL and X-ray elongated distributions. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2255. A relaxed-appearing X-ray emission with WL substructures. WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2061. A dissociative merger with a radio relic that is very distant from the X-ray brightness peak. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2034. A dissociative merger with a bullet shape. WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: RXCJ1314. A merging system with a possibly large viewing angle and radio relics at asymmetric projected separation. WL contours start at 3σ and increase in steps of 0.5σ. A candidate background cluster (BG Cluster) is detected in the south with a spectroscopically confirmed z = 0.47 galaxy in the center of the mass contours.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: ZwCl1447. A merging system with double radio relics. WL contours start at 3σ and increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: ZwCl1856. An equal-mass merger with low total mass and double radio relics. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: MACSJ1149. A high-z cluster with a north–south elongation in the mass and X-ray distributions. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: PLCKG287. A centrally dominant, massive cluster with low-mass subclusters and double radio relics at asymmetric projected separation. WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: PSZ1G108. A centrally dominant cluster with large separation double radio relics. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: ZwCl0008. A dissociative merger of equal-mass subclusters. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: MACSJ1752. An equal-mass merger with ram-pressure-stripped tails in the X-ray emission and double radio relics. WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: CIZAJ2242 (The Sausage Cluster). A system with a textbook, arc-shaped radio relic, complex X-ray emission, and a bimodal mass distribution. WL contours increase in steps of 1σ.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: The fitting result of Spec-Unet under different noise influences. The black line represents the spectral flux, the red line is the pseudocontinuum fitted by Spec-Unet, and the gray dashed line represents the ±1σflux. The first row is the emission line containing NALs, the second row is the emission line with BALs, the third row is the emission line without absorption features, while the fourth and fifth rows are those without obvious emission lines.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: Examples of poor Spec-Unet fitting. The black line represents the spectral flux, the red line is the pseudocontinuum fitted by Spec-Unet, and the gray dashed line represents the ±1σflux. Both spectra contain extreme BAL, which Spec-Unet cannot handle well.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Observed composite spectrum of RM 102. The regions between the vertical black and brown dashed lines represent the broad UV and optical wavelength ranges, respectively, considered in this work. The shaded blue and red regions denote the blue and red parts in the corresponding regions. Top panel: the observed spectrum is in gray, the dashed red and the blue lines correspond to the best fit of the emission lines and the continuum, respectively. The dashed black line represents the Balmer continuum, and the green line denotes the contribution of starlight. Bottom panel: the red line depicts the Fe II pseudocontinuum. For reference, we also show the semiempirical UV (dotted line) and optical (dashed line) templates implemented in PyQSOfit in dark red.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Contour plots for the EW of optical Fe II blends for microturbulence Vturb = 100 km s−1.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Contour plots for the EW of UV Fe II blends without microturbulence. We only plot contours with EW greater than the observed EW.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Contour plots for the EW of UV Fe II blends for microturbulence Vturb = 100 km s−1.
Paper: New Theoretical Fe II Templates for Bright Quasars
Authors: Ashwani Pandey, Mary Loli Martínez-Aldama, Bożena Czerny, Swayamtrupta Panda, Michal Zajaček, Jian-Min Wang, Yan-Rong Li, Pu Du
Figure caption: Contour plots for the EW of optical Fe II blends without microturbulence.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The left panel is the waiting time (time interval between two successive bursts observed by GECAM-B/C) of the X-ray bursts vs. their occurring times, where the time of the FRB 20221014 is represented by the green dashed line. The right panel is the distribution of waiting time. The horizontal dotted lines represent the best-fit lognormal function with a mean of ﹩338.8{4}_{-212.95}^{+573.16}﹩ s for GECAM-B and ﹩79.4{3}_{-51.89}^{+149.65}﹩ s for GECAM-C, respectively.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: Representative examples of GECAM-detected bursts of SGR J1935+2154. For each burst, light curves are shown for high gain (HG, 6–300 keV). The background of each burst is shown by the red dotted line. The green vertical dotted line and blue dotted line are assessed by the Bayesian block algorithm.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The left panel is the burst duration of each burst observed by GECAM-B/C. The right panel is the burst duration distributions of GECAM-B/C. The horizontal dotted lines show the best-fit lognormal function with a mean value listed in Table 5.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The burst history of SGR J1935+2154 observed by GECAM-B/C.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The evolution of hardness ratio of each burst in 50–200/40–50 keV for GECAM-B and 30–200/15–30 keV for GECAM-C.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: Lomb–Scargle periodogram of X-ray bursts from SGR J1935+2154 observed by GECAM. The vertical red dotted line indicates the peak of periodogram, which is 134.63 days.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: Phase-folded burst rate according to the 134.63 day period with MJD 59215 (2021 January 1) referenced as phase 0. The active window (i.e., from ϕ = 0.7 to ϕ = 1.5) is denoted with red dotted lines.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The significance of burst vs. angle separation between the targeted-search location (TL) and the true position of SGR J1935+2154.
Paper: GECAM Observations of the Galactic Magnetar SGR J1935+2154 during the 2021 and 2022 Burst Active Episodes. I. Burst Catalog
Authors: Sheng-Lun Xie, Ce Cai, Yun-Wei Yu, Shao-Lin Xiong, Lin Lin, Yi Zhao, Shuang-Nan Zhang, Li-Ming Song, Ping Wang, Xiao-Bo Li, Wang-Chen Xue, Peng Zhang, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Yue Wang, Zheng-Hang Yu, Pei-Yi Feng, Jin-Peng Zhang, Shuo Xiao, Hai-Sheng Zhao, Wen-Long Zhang, Yan-Ting Zhang, Yue Huang, Xiao-Yun Zhao, Xiang Ma, Shi-Jie Zheng, Xin-Qiao Li, Xiang-Yang Wen, Ke Gong, Zheng-Hua An, Da-Li Zhang, Sheng Yang, Xiao-Jing Liu, Fan Zhang
Figure caption: The burst duration of 14 X-ray bursts observed by both GECAM-B and GECAM-C.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolutions of the abundances of NH2CH2CH2OH, HOCH2CN, CH3OH, C2H5OH, and C2H3OH, as well as their ice-phase species s-NH2CH2CH2OH, s-HOCH2CN, s-CH3OH, s-C2H5OH, and s-C2H3OH, in the best-fitting isothermal model I5 (a) and C-shock model S5 (b). The gray dashed line presents the time-varying temperature T(S5). The vertical gray area supplies the “consistent timescale.” The horizontal red, black, green, blue, and orange areas display the observed constraints of NH2CH2CH2OH, HOCH2CN, CH3OH, C2H5OH, and C2H3OH relative to the total hydrogen density, respectively.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolutions of the abundances of NH2CH2CH2OH, HOCH2CN, CH3NH2, NH2OH, CH3OH, C2H5OH, and C2H3OH in C-shock models S1–S6. The horizontal red, blue, black, olive, green, cyan, and orange areas present their observational constraints relative to the total hydrogen column density, respectively. Gray dashed lines present the time-varying temperatures T(Sn). The vertical gray areas supply the “consistent timescales” between the modeled physical conditions and their observed values (temperature: 30–150 K; H2 density: 104–105 cm−3).
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolutions of the modeled abundance ratios NH2CH2CH2OH/HOCH2CN, NH2CH2CH2OH/CH3NH2, NH2CH2CH2OH/NH2OH, NH2CH2CH2OH/CH3OH, NH2CH2CH2OH/C2H5OH, NH2CH2CH2OH/C2H3OH, NH2OH/C2H3OH, C2H3OH/CH3OH, and C2H3OH/C2H5OH in C-shock models S5 and S6. The horizontal cyan, red, blue, green, orange, black, olive, purple, and pink areas stand for their observed abundance ratios with uncertainties, respectively. Gray dashed lines present the time-varying temperatures T(S5) and T(S6). The vertical gray areas supply the “consistent timescales.”
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolutions of the abundances of NH2CH2CH2OH, HOCH2CN, CH3NH2, NH2OH, CH3OH, C2H5OH, and C2H3OH in C-shock models S7–S9 and S16–S18. The horizontal red, blue, black, olive, green, cyan, and orange areas present their observational constraints relative to the total hydrogen column density, respectively. Gray dashed lines present the time-varying temperatures T(Sn). The vertical gray areas supply the “consistent timescales.”
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolution of temperature (T) in the warm-up model with the final temperature ﹩{T}_{{\rm{\max }}}﹩ = 200 K (left panel) and temporal evolutions of total hydrogen density (nH) and visual extinction (AV) in the free-fall collapse and warm-up models (right panel).
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Temporal evolutions of temperatures T, total hydrogen densities nH, and visual extinctions AV in C-shock models S1–S18.
Paper: Chemistry of NH2CH2CH2OH and Its Related Species in the Interstellar Medium
Authors: Guoming Zhao, Mingwei He, Donghui Quan, Xue Yang, Long-Fei Chen, Dalei Li, Qiang Chang, Yuxuan Wu, Yanze Teng, Yisheng Qiu, Xinke He, Ming-Shuo Ma, Minglei Qu
Figure caption: Linear fit of 16 interaction energies calculated with one water molecule against the experimental binding energies.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: Projected separation of the BCGs (blue stars), luminosity peaks (red squares), and number density peaks (green ) from the WL peak. The horizontal gray bars represent the uncertainty on the mass peak position. The vertical colored lines show the median separations of each luminous tracer from the mass peak and their 68% uncertainty.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: WL mass–σv scaling relation for subclusters of merging systems that exhibit radio relics. Masses and system index letters are from Table 4. The black dashed line is the A. E. Evrard et al. (2008) scaling relation. WL mass estimates are preferentially lower than the A. E. Evrard et al. (2008) relation, especially at the low-mass end. ZWCL2341–NW and A2034–SW have very low velocity dispersions (359 ± 39 and 366 ± 55 km s−1, respectively) and are not shown here but are included in the analysis.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: Mass ratio of merging clusters that exhibit radio relics. Masses are from the 2PNFW method. Masses and system index letters are from Table 4. The solid (dashed) black line represents the 1:1 (1:4) mass ratio. Most of the radio relic systems are in major mergers (ratio < 4). Twenty-two of the systems are shown here (omitting A746, A781, A1300, and MACSJ1149).
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: Comparison of the mass derived from the A. R. Duffy et al. (2008) c–M relation to the mass derived from the two-parameter fit (values from Table 4). The black dashed line represents the 1:1 relation. The fuchsia line is the best-fit linear regression. Uncertainties are considered on both axes.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: ZwCl2341. A complex cluster merger with a bullet-shaped X-ray emission. WL contours increase in steps of 0.5σ.
Paper: Deep Learning–based Pseudocontinuum Fitting of C IV Emission-line Regions for High-quality Absorption-line Measurement
Authors: Ming-Liang Yao, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Wei-Rong Huang
Figure caption: Histogram of the ratio of EW and FWHM parameters. (a) Histogram showing the ratio of EW between HUANG23’s pseudocontinuum followed by NALs fitted and EW from fitted Spec-Unet’s pseudocontinuum, with values centered mainly around 1.0, indicating substantial agreement. (b) The consistency is further illustrated through the ratios of FWHM for NALs derived from both methods, also clustering near 1.0; blue represents the FWHM1548, and red represents the FWHM1551. These figures collectively demonstrate a high degree of similarity in results between HUANG23’s and Spec-Unet spectra feature analysis.