adsabs/AstroCLIMB huggingface dataset:
Paper: Improvement of Pan-STARRS Photometric Calibration with LAMOST and Gaia
Authors: Kai Xiao, Haibo Yuan, Bowen Huang, Ruoyi Zhang, Lin Yang, Shuai Xu
Figure caption: A zoom-in plot for a small region in Figure 4 in the i band. A color bar is overplotted to the right. Note that the region is the same as Figure 8 of Xiao & Yuan (2022), but for the XPSP results.
Paper: Improvement of Pan-STARRS Photometric Calibration with LAMOST and Gaia
Authors: Kai Xiao, Haibo Yuan, Bowen Huang, Ruoyi Zhang, Lin Yang, Shuai Xu
Figure caption: Spatial variations of the magnitude offsets of the SCR (left panel) and SCR′ (right panel) methods for the common stars in the g, r, i, z, and y bands in the Equatorial coordinate system. Color bars are overplotted to the bottom. The HEALPix index is level 8.
Paper: Improvement of Pan-STARRS Photometric Calibration with LAMOST and Gaia
Authors: Kai Xiao, Haibo Yuan, Bowen Huang, Ruoyi Zhang, Lin Yang, Shuai Xu
Figure caption: Histogram distributions of derived magnitude offsets from the XPSP method after ﹩14^{\prime} \times 14^{\prime} ﹩ binning. From left to right are the g, r, i, z, and y bands. The red dotted curves are the Gaussian fitting results, with mean and sigma values labeled in the top left corners.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe XV. Bernhardt refers to Bernhardt et al. (2014), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe XIV. Hahn refers to Hahn et al. (2013), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe IX. Hahn refers to Hahn et al. (2016), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe X. Hahn refers to Hahn et al. (2012c), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe VIII. Hahn refers to Hahn et al. (2015), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe XI. Hahn refers to Hahn et al. (2012c), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe XIII. Hahn refers to Hahn et al. (2011a, 2012b), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe XII. Hahn refers to Hahn et al. (2011b), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe XVII. Hahn refers to Hahn et al. (2013), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: Improvement of Pan-STARRS Photometric Calibration with LAMOST and Gaia
Authors: Kai Xiao, Haibo Yuan, Bowen Huang, Ruoyi Zhang, Lin Yang, Shuai Xu
Figure caption: 2D third-order polynomial fitting (with 10 free parameters) of temperature as a function of ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ and [Fe/H] for around 110,000 stars. The left panel shows the fitting results: the red and blue curves represent results for [Fe/H] = 0 and −1, respectively, and the fitting residuals are labeled. The middle and right panel plot residuals against ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ and [Fe/H] , respectively. The black dotted lines denote residuals of 0.
Paper: Improvement of Pan-STARRS Photometric Calibration with LAMOST and Gaia
Authors: Kai Xiao, Haibo Yuan, Bowen Huang, Ruoyi Zhang, Lin Yang, Shuai Xu
Figure caption: Left panels: spatial distribution of the stars. Middle panels: differences between the XPSP standardized magnitudes and the PS1 magnitudes. Right panels: differences between the XPSP standardized magnitudes and the aperture magnitudes of PS1. From top to bottom are the g, r, i, z, and y bands, respectively. Color bars are overplotted to the right.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: A table showing the ions that are included in the CHIANTI version 10.1 database.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: BTI scaled ionization cross sections of S XIII. Hahn refers to Hahn et al. (2012a), and fit to the DI cross section refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Mg VIII. Hahn refers to Hahn et al. (2010), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of S XIII. Hahn refers to Hahn et al. (2012a), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of Fe XVIII. Hahn refers to Hahn et al. (2013), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: CHIANTI—An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recombination Rates and Other Updates 
Authors: Kenneth P. Dere, G. Del Zanna, P. R. Young, E. Landi
Figure caption: Ionization cross sections of O V. Fogle refers to Fogle et al. (2008), 2007 refers to Dere (2007), and present refers to the results reported here.
Paper: A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J = 2–1 Data Analysis
Authors: Y. P. Zou, 益鹏 邹, J. S. Zhang, 江水 张, C. Henkel, D. Romano, W. Liu, 玮 刘, Y. H. Zheng, 映慧 郑, Y. T. Yan, 耀庭 闫, J. L. Chen, 家梁 陈, Y. X. Wang, 友鑫 汪, J. Y. Zhao, 洁瑜 赵
Figure caption: A prominent radial 18O/17O gradient is confirmed by our HMSFR sample, encompassing 72 sources with accurate distance values. Red and gray indicate the results from J = 2–1 and J = 1–0 data (the latter taken from Paper I), respectively. The dashed lines represent unweighted linear fits, while the expressions give the fitting parameters. As in Figure 6(a), the curve represents predictions of the GCE model including both rotating stars and novae (MWG-12 in Romano et al. 2019).
Paper: A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J = 2–1 Data Analysis
Authors: Y. P. Zou, 益鹏 邹, J. S. Zhang, 江水 张, C. Henkel, D. Romano, W. Liu, 玮 刘, Y. H. Zheng, 映慧 郑, Y. T. Yan, 耀庭 闫, J. L. Chen, 家梁 陈, Y. X. Wang, 友鑫 汪, J. Y. Zhao, 洁瑜 赵
Figure caption: A comparison of isotope ratios from our J = 1–0 (Paper I) and J = 2–1 (this paper) data. Red and gray indicate IRAM and SMT J = 2–1 data, respectively. For the green line and shaded areas, see the caption to Figure 5.
Paper: A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J = 2–1 Data Analysis
Authors: Y. P. Zou, 益鹏 邹, J. S. Zhang, 江水 张, C. Henkel, D. Romano, W. Liu, 玮 刘, Y. H. Zheng, 映慧 郑, Y. T. Yan, 耀庭 闫, J. L. Chen, 家梁 陈, Y. X. Wang, 友鑫 汪, J. Y. Zhao, 洁瑜 赵
Figure caption: A comparison of the 18O/17O ratios from our J = 1–0 and J = 2–1 data for 24 sources. The left and right panel are before and after correction of the RADEX calculations, respectively. The green line and shaded areas are the same as Figure 5.
Paper: A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J = 2–1 Data Analysis
Authors: Y. P. Zou, 益鹏 邹, J. S. Zhang, 江水 张, C. Henkel, D. Romano, W. Liu, 玮 刘, Y. H. Zheng, 映慧 郑, Y. T. Yan, 耀庭 闫, J. L. Chen, 家梁 陈, Y. X. Wang, 友鑫 汪, J. Y. Zhao, 洁瑜 赵
Figure caption: The C18O/C17O integrated intensity ratio as a function of 13CO/C18O for the J = 2–1 transition.
Paper: A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J = 2–1 Data Analysis
Authors: Y. P. Zou, 益鹏 邹, J. S. Zhang, 江水 张, C. Henkel, D. Romano, W. Liu, 玮 刘, Y. H. Zheng, 映慧 郑, Y. T. Yan, 耀庭 闫, J. L. Chen, 家梁 陈, Y. X. Wang, 友鑫 汪, J. Y. Zhao, 洁瑜 赵
Figure caption: The Ratio1–0/Ratio2–1 values are plotted as a function of Ratio1–0. Red and gray indicate IRAM and SMT J = 2–1 data, respectively.
Paper: A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J = 2–1 Data Analysis
Authors: Y. P. Zou, 益鹏 邹, J. S. Zhang, 江水 张, C. Henkel, D. Romano, W. Liu, 玮 刘, Y. H. Zheng, 映慧 郑, Y. T. Yan, 耀庭 闫, J. L. Chen, 家梁 陈, Y. X. Wang, 友鑫 汪, J. Y. Zhao, 洁瑜 赵
Figure caption: Spectra of the sources without effective measurements of C18O/C17O.                    1 of 3 image
Paper: General Physical Properties of Fermi Blazars
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Xiaogu Zhong, 晓谷 钟, Hongyu Liu, 红宇 刘, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: Relation between radiation jet power (top), jet kinetic power (bottom), and accretion disk luminosity for Fermi blazars. The red dots are FSRQs and the green dots are BL Lacs. The meaning of the solid and dashed lines is the same as in Figure 4. In the bottom plot, the pink solid line represents the one-to-one correlation. The relation between jet kinetic power, jet radiation power, and accretion disk luminosity for Fermi blazars is ﹩\mathrm{log}{P}_{\mathrm{rad}}﹩ = ﹩(0.31\pm 0.06)\mathrm{log}{L}_{\mathrm{disk}}+(29.95\pm 2.91)﹩ and ﹩\mathrm{log}{P}_{\mathrm{jet}}﹩ = ﹩(0.19\pm 0.04)\mathrm{log}{L}_{\mathrm{disk}}+(37.46\pm 1.79)﹩, respectively.
Paper: General Physical Properties of Fermi Blazars
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Xiaogu Zhong, 晓谷 钟, Hongyu Liu, 红宇 刘, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: Relation between L bol/L Edd and P jet/L bol. The red dots are FSRQs and the green dots are BL Lacs. Solid line: maximal jet power ﹩{P}_{\mathrm{BP}}^{\max }﹩ extracted from a standard accretion disk (the Blandford–Payne mechanism). Dashed line: maximal jet power ﹩{P}_{\mathrm{BZ}}^{\max }﹩ extracted from a rapidly spinning black hole a = 0.95 (the Blandford–Znajek mechanism).
Paper: General Physical Properties of Fermi Blazars
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Xiaogu Zhong, 晓谷 钟, Hongyu Liu, 红宇 刘, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: Relation between jet kinetic power and black hole mass. The red dots are FSRQs and the green dots are BL Lacs. The meaning of the solid and dashed lines is the same as that of Figure 4.