adsabs/AstroCLIMB huggingface dataset:
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 gamma-ray luminosity (top) and radio luminosity (bottom) and jet kinetic power 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.
Paper: A Coronal Mass Ejection Source Region Catalog and Their Associated Properties
Authors: Satabdwa Majumdar, Ritesh Patel, Vaibhav Pant, Dipankar Banerjee, Aarushi Rawat, Abhas Pradhan, Paritosh Singh
Figure caption: The distributions of the longitudes of the source regions are plotted for all CMEs in panel (a) and for the CMEs coming from ARs, APs, and PEs in panels (b), (c), and (d), respectively. The shaded regions in each plot highlight the importance of the STEREO mission in identifying and locating the source regions at the backside of the Sun (with respect to the Sun–Earth line).
Paper: A Coronal Mass Ejection Source Region Catalog and Their Associated Properties
Authors: Satabdwa Majumdar, Ritesh Patel, Vaibhav Pant, Dipankar Banerjee, Aarushi Rawat, Abhas Pradhan, Paritosh Singh
Figure caption: Distributions of the position angles of the CMEs are plotted for all CMEs in panel (a) and for the CMEs coming from ARs, APs, and PEs in panels (b), (c), and (d), respectively.
Paper: A Coronal Mass Ejection Source Region Catalog and Their Associated Properties
Authors: Satabdwa Majumdar, Ritesh Patel, Vaibhav Pant, Dipankar Banerjee, Aarushi Rawat, Abhas Pradhan, Paritosh Singh
Figure caption: The distributions of the longitudes of all CMEs are plotted for the rising, maximum, and declining phases of cycle 23 in panels (a), (b), and (c), respectively, and similarly for cycle 24 in panels (d), (e), and (f).
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: (Top) L X against F XO for galaxies and QSOs from the spec-z sample. The left and right panels are the same, except for (left) galaxies on top of QSOs or (right) QSOs on top of galaxies to visualize both subsamples clearly. The dashed red line is a linear relation that fits the galaxy sample. The blue line separates galaxies from QSOs. (Bottom) The same, but with L X against L  r . The blue line is the best-fit relation for QSOs.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: Top: WISE spec-z color–color plot for galaxies and QSOs. Bottom: comparison of WISE spec-z and photo-z samples. The left and right panels are the same, but the different objects are drawn on top to visualize both samples clearly. The dashed blue line is for W12 = 0.8, often used to identify QSOs without galaxy contaminations. The dashed red line is for W12 = 0.4, which we apply to select galaxies without QSO contaminations.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: (Left) Optical r mag against X-ray flux for the SDSS spec-z sample. The diagonal lines indicate F XO values of 0.01, 0.1, and 10 from the lower left to the upper right. (Right) F XO distribution for the QSO, galaxy, and star subsamples.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption:  L X against (top) F XO and (bottom) L  r  from spec-z and photo-z samples. The left and right panels are the same, except for (left) the spec-z sample on top of the photo-z sample or (right) vice versa to visualize both samples clearly. The diagonal lines are the same as in Figure 5.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: The optical, IR, and UV counterparts of CSC2 sources plotted in Galactic coordinates (l, b).
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption:  L X against WISE color W12 (= W1–W2) (top) for galaxies and QSOs from the SDSS spec-z sample (bottom) from the SDSS spec-z and photo-z samples. The left and right panels are the same, but the different objects are drawn on top to visualize both samples clearly. The vertical lines are the same as in Figure 7. The blue line separates galaxies and QSOs.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: X-ray sources in CSC2 are plotted in Galactic coordinates (l, b). A few well-known objects are also marked.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: The redshift and L X distributions of galaxies and QSOs for the SDSS spec-z sample.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: False-match fractions as a function of optical and IR source density. (Top left) Applying the initial maximum separation of 10″ without further selection by separation, and (top right) applying an additional selection with a separation <3″. In both cases, we set p_any > 0.5. (Bottom panel) Same as the top panel, but with p_any > 0.8. The crosses indicate the ensembles with a relatively small number of counterparts (≾10), which are less significant. The horizontal lines indicate that the false-positive rate is 5%, a typical limit in this work.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: (Left) Comparison of SDSS spec-z and photo-z. (Right) Poor-quality measurements are excluded by selecting only those with zWarning = 0 (for spec-z), photoErrorClass = 1 (for photo-z), and z / error(z) > 2 (for all).
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: The total number and density (in arcmin2) of X-ray, optical, and IR sources in each ensemble. Unique colors and line styles mark different catalogs (see legend). The ensembles used in the simulation are marked by the color and line style of the catalogs by the small vertical bars at the top of the figure.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: (Left) Pan-STARRS photo-z and (right) Legacy photo-z are compared with SDSS spec-z. Poor-quality measurements are excluded by selecting only those with zWarning = 0 (for SDSS spec-z), extrapolationClass = extrapolationPhotoz = 0 (for Pan-STARRS photo-z), and error(z)/z < 0.5 (for all).
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption:  L X against W12 for (left) the PS–WISE sample and (right) the LS–WISE sample. All lines are the same as in Figure 8.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: (Left) Pan-STARRS photo-z and (right) Legacy photo-z are compared with SDSS photo-z. Poor-quality measurements are excluded by selecting only those with photoErrorClass = 1 (for SDSS photo-z), extrapolationClass = extrapolationPhotoz = 0 (for Pan-STARRS photo-z), and error(z)/z < 0.5 (for all).
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption:  L X against F XO for (left) the PS and (right) the LS samples. All lines are the same as in the top panel of Figure 6.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: W12 (W1–W2) against W23 (W2–W3) for (left) the PS–WISE sample and (right) the LS–WISE sample. All lines are the same as in Figure 7.
Paper: The Chandra Source Catalog Normal Galaxy Sample
Authors: Dong-Woo Kim, Alyssa Cassity, Binod Bhatt, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan, Arnold Rots
Figure caption: (Left) The Pan-STARRS r mag and (right) the Legacy r mag are compared with the SDSS r mag.
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 2022 refers to the results reported here. Also plotted is the MB velocity distribution for a temperature of 1.91 MK, and m〈v〉2/2 for the same temperature is displayed as a vertical line.
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: Top: Ionization rate coefficients of Fe XIV. The label 2007 refers to Dere (2007), and present refers to the present results. Bottom: The ratio of the present rate coefficients to those of 2007.
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: The revised ionization balance for Fe ions for stages X–XIV. The full line represents the present calculation and the dashed line the version 10.0 calculation
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 IRAM 30 m spectra of C18O (upper panels) and C17O (lower panels) with green fit lines of the 96 sources detected in both isotopologues.                 1 of 4 image
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 SMT 10 m spectra of C18O (upper panels) and C17O (lower panels) with green fit lines of the 325 sources detected in both isotopologues.                 1 of 11 image
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: Top panels: the 28Si abundances in the ejecta are shown with respect to the explosion temperature peak (continuous black line) for the models T1.4Z0 (Z met = 0, left), T1.4Z0.014 (Z met = 0.014, middle), and T1.4Z0.1 (Z met = 0.1, right). 28Si abundances are shown with contributions from radioactive species, which are negligible in this case. Middle panels: the same as for top panels, but for models S1.0Z0, S1.0Z0.014, and S1.0Z0.1, respectively. Bottom panels: the same as for top panels, but for models M0.8Z0, M0.8Z0.014, and M0.8Z0.1, respectively.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: Production factors for models T1.4Z0 (top), T1.4Z0.014 (middle), and T1.4Z0.1 (bottom).
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The ejected mass for Si and its stable isotopes 28Si, 29Si, and 30Si are shown at different metallicities. The radiogenic contributions are included in the elemental yields. Decayed and undecayed abundances are shown for isotopes (continuous lines with crosses and dotted–dashed lines with empty circles, respectively). Data is presented for sets T1.4 (upper panel), S1.0 (middle panel), and M0.8 (lower panel).
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: As in Figure 4 but for the ejected mass of Ar, and its stable isotopes 36Ar, 38Ar, and 40Ar.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of Ca, and its stable isotopes 40Ca, 42Ca, 43Ca, and 44Ca.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of S, and its stable isotopes 32S, 33S, 34S, and 36S.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: Production factors for models M0.8Z0, M0.8Z0.014, and M0.8Z0.1.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: Isotopic production factors for models S1.0Z0, S1.0Z0.014, and S1.0Z0.1.
Paper: A White Dwarf Search Model Based on a Deep Transfer-learning Method
Authors: Lei Tan, 磊 谈, Zhicun Liu, 志 存 柳, Feng Wang, 锋 王, Ying Mei, 盈 梅, Hui Deng, 辉 邓, Chao Liu, 超 刘
Figure caption: Examples of the samples labeled as white dwarfs in LAMOST that were not identified as white dwarfs by our model.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of Fe, and its stable isotopes 54Fe, 56Fe, 57Fe, and 58Fe.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of Ni, and its stable isotopes 58Ni, 60Ni, 61Ni, 62Ni, and 64Ni.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of 55Mn.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of Cr, and its stable isotopes 50Cr, 52Cr, 53Cr, and 54Cr.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: As in Figure 4 but for ejected mass of Ti, and its stable isotopes 46Ti, 47Ti, 48Ti, 49Ti, and 50Ti.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of 59Co.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of Zn, and its stable isotopes 64Zn, 66Zn, 67Zn, and 68Zn. There is no production of zinc in the M0.8 models, and therefore the plot is omitted.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The same as in Figure 4 but for the ejected mass of V, and its stable isotopes 50V and 51V.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: Ejected mass of 56Ni as a function of initial metallicity for our models, compared with Timmes et al. (2003) calculations.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: Comparison with the T1.4 yields T1.4Z0.014 (upper panel), S1.0Z0.014 (middle panel), and M0.8Z0.014 (lower panel). In each case, the metallicity closest to the metallicity used in the parent model is selected from our grid of initial 22Ne mass fractions
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: The fraction of the total jet power transformed into radiation (top), relativistic electrons (middle), and Poynting flux (bottom). The red dots are FSRQs and the green dots are BL Lacs.
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: The Doppler factor vs. synchrotron-peak frequency for Fermi blazars. The gray circles show FSRQs; the blue squares show other BL Lacs; the red triangles show HBLs.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: Yields from Gronow et al. (2020, green circles) compared with our S1.0Z0 model (black squares, upper panel), and Leung & Nomoto (2020) compared with model S1.0Z0.014 (lower panel).
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: The example of broadband SEDs of 3C345 is modeled by using a one-zone model.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The upper panel shows W7 decayed elemental abundances from Nomoto & Leung (2018; green circles) compared with T1.4Z0.014 (black line, square markers). In the lower panel, the yields from Seitenzahl et al. (2013b) are compared instead.
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: The distribution of physical parameters. The jet kinetic power is P jet = P B + P e + P p. The red line is FSRQs and the green line is BL Lacs.
Paper: Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
Authors: James D. Keegans, Marco Pignatari, Richard J. Stancliffe, Claudia Travaglio, Samuel Jones, Brad K. Gibson, Dean M. Townsley, Broxton J. Miles, Ken J. Shen, Gareth Few
Figure caption: The 0.81 M ⊙ model from Sim et al. (2010, green circles) compared with our M0.8Z0 model (black squares, upper panel) and the 0.88 M ⊙ model S1.0 from the same publication (lower panel).
Paper: A Coronal Mass Ejection Source Region Catalog and Their Associated Properties
Authors: Satabdwa Majumdar, Ritesh Patel, Vaibhav Pant, Dipankar Banerjee, Aarushi Rawat, Abhas Pradhan, Paritosh Singh
Figure caption: The distributions of the differences between the latitudes of the source regions of the CMEs and the position-angle equivalent latitudes of the CMEs, occurring during the rising, maximum, and declining phases of Cycle 23 (horizontally for each row), are plotted for CMEs originating from ARs, APs, and PEs (vertically for each column, corresponding to each phase of the solar cycle). A Gaussian is also fitted to each of the nine cases and the mean (μ), the absolute mean (μ  a ), and the standard deviation (σ) for each of the fitted Gaussians are also shown in each plot.
Paper: A Coronal Mass Ejection Source Region Catalog and Their Associated Properties
Authors: Satabdwa Majumdar, Ritesh Patel, Vaibhav Pant, Dipankar Banerjee, Aarushi Rawat, Abhas Pradhan, Paritosh Singh
Figure caption: Latitudinal deflections of CMEs are plotted for all the CMEs in panel (a) and for the CMEs coming from ARs, APs, and PEs in panels (b), (c), and (d), respectively. In each panel, the top part shows the distribution of the latitude of the source region, with a double-peak signature in all four cases. Distributions of the position-angle equivalent latitudes are plotted in the bottom parts.