adsabs/AstroCLIMB huggingface dataset:
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: Lyα stacks of MUSE data cubes for all HAEs in our sample, as well as the LAE and non-LAE subsamples. All data cubes are normalized by the intrinsic Hα flux following the Calz dust attenuation law. The psedo-Lyα narrowband (NB) images in the left cover 1213–1219 Å, i.e., slices of ±3 Å centered on 1216 Å; the continuum (Cont. for short) NB images are calculated from 1230 to 1240 Å slices and scale to the wavelength width of Lyα slices. The extracted spectra based on r = 2.″5 circular apertures (black solid circle in Lyα NB images) are shown, with the best-fit skewed Gaussian profiles in red.
Paper: Application of Deep-learning Methods for Distinguishing Gamma-Ray Bursts from Fermi/GBM Time-tagged Event Data
Authors: Peng Zhang, 鹏 张, Bing Li, 兵 李, Renzhou Gui, 任舟 桂, Shaolin Xiong, 少林 熊, Ze-Cheng Zou, 泽城 邹, Xianggao Wang, 祥高 王, Xiaobo Li, 小波 李, Ce Cai, 策 蔡, Yi Zhao, 一 赵, Yanqiu Zhang, 艳秋 张, Wangchen Xue, 王陈 薛, Chao Zheng, 超 郑, Hongyu Zhao, 宏宇 赵
Figure caption: Four representative samples from the data set. The GRBs with a single peak (GRB 200323782, n7), two peaks (GRB 160802259, n2), low S/N (GRB 180927993, n5), and complex structure (GRB 160912521, nb) are represented. For each panel, the upper subpanel shows the normalized count map (model input), the middle subpanel shows the normalized light curve of the full energy band, and the lower subpanel is the feature heat map generated by Grad-CAM method. The red dashed line represents the trigger time of Fermi, and the gray area indicates the Fermi-T 90.
Paper: Application of Deep-learning Methods for Distinguishing Gamma-Ray Bursts from Fermi/GBM Time-tagged Event Data
Authors: Peng Zhang, 鹏 张, Bing Li, 兵 李, Renzhou Gui, 任舟 桂, Shaolin Xiong, 少林 熊, Ze-Cheng Zou, 泽城 邹, Xianggao Wang, 祥高 王, Xiaobo Li, 小波 李, Ce Cai, 策 蔡, Yi Zhao, 一 赵, Yanqiu Zhang, 艳秋 张, Wangchen Xue, 王陈 薛, Chao Zheng, 超 郑, Hongyu Zhao, 宏宇 赵
Figure caption: Schematic diagram of our CNN architectures. The numbers at the top and bottom of Conv-block denote the convolutional stride (default is 1) and number of convolutional kernels, respectively. The number at the bottom of the figure describes the variation of the length and width of the feature maps.
Paper: Application of Deep-learning Methods for Distinguishing Gamma-Ray Bursts from Fermi/GBM Time-tagged Event Data
Authors: Peng Zhang, 鹏 张, Bing Li, 兵 李, Renzhou Gui, 任舟 桂, Shaolin Xiong, 少林 熊, Ze-Cheng Zou, 泽城 邹, Xianggao Wang, 祥高 王, Xiaobo Li, 小波 李, Ce Cai, 策 蔡, Yi Zhao, 一 赵, Yanqiu Zhang, 艳秋 张, Wangchen Xue, 王陈 薛, Chao Zheng, 超 郑, Hongyu Zhao, 宏宇 赵
Figure caption: The learning curve of nine single-network models. Due to the training mechanism of early stopping, the epoch at which the model stops varies.
Paper: Application of Deep-learning Methods for Distinguishing Gamma-Ray Bursts from Fermi/GBM Time-tagged Event Data
Authors: Peng Zhang, 鹏 张, Bing Li, 兵 李, Renzhou Gui, 任舟 桂, Shaolin Xiong, 少林 熊, Ze-Cheng Zou, 泽城 邹, Xianggao Wang, 祥高 王, Xiaobo Li, 小波 李, Ce Cai, 策 蔡, Yi Zhao, 一 赵, Yanqiu Zhang, 艳秋 张, Wangchen Xue, 王陈 薛, Chao Zheng, 超 郑, Hongyu Zhao, 宏宇 赵
Figure caption: The confusion matrices of nine single-network models.
Paper: Application of Deep-learning Methods for Distinguishing Gamma-Ray Bursts from Fermi/GBM Time-tagged Event Data
Authors: Peng Zhang, 鹏 张, Bing Li, 兵 李, Renzhou Gui, 任舟 桂, Shaolin Xiong, 少林 熊, Ze-Cheng Zou, 泽城 邹, Xianggao Wang, 祥高 王, Xiaobo Li, 小波 李, Ce Cai, 策 蔡, Yi Zhao, 一 赵, Yanqiu Zhang, 艳秋 张, Wangchen Xue, 王陈 薛, Chao Zheng, 超 郑, Hongyu Zhao, 宏宇 赵
Figure caption: Overall architecture of the fused model.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption:  R–L relations for the four broad lines in this work. In each panel, the red dashed line shows the most recent literature relation (Bentz et al. 2013; Kaspi et al. 2021; Yu et al. 2023). The light blue lines are random draws from the linear regression of predicting ﹩\mathrm{log}\tau ﹩ with ﹩\mathrm{log}L﹩ using the Bayesian approach in Kelly (2007). The blue dashed line is a forced regression fit with slope fixed to that measured in earlier work. Overall, measured SDSS-RM lags follow these earlier relations, but there are notable deviations (in particular for C IV). Our lag measurements suggest that the Hβ and Mg II R–L relations are reasonably tight (with an intrinsic scatter of ∼0.3 dex in lag), while the C IV R–L relation has substantially larger scatter (∼0.5 dex) than the other two lines. The Spearman rank-order test results on the SDSS-RM sample (correlation coefficient ρ and p-value p) are marked in each panel. These results are discussed in detail in Section 5.1 and Table 4.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Comparisons between M RM and M SE (using earlier SE recipes) for the same line. Hβ has the best correlation while C IV has the worst correlation. However, for all three lines, there are good correlations between σ line,rms and FWHMmean, so the poor mass correlation for C IV is mainly driven by the poor R–L relation. Because the single-epoch mass is solely determined by continuum luminosity and line width, its dynamic range can be artificially suppressed compared with RM-based masses (Shen 2013). In the bottom panels, the blue dotted line is a simple median of the residuals, rather than the average offset weighted by measurement uncertainties.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Same as Figure 14, but for the comparisons between M RM and updated M SE estimates (Table 4) for the same line. The new Mg II SE recipe is now an approximately unbiased estimator (i.e., at a given RM mass, they return an unbiased expectation value), while the Hβ and C IV SE recipes are still biased estimators (as we adopted similar slopes on L and mean FWHM as the earlier recipe in Vestergaard & Peterson 2006). However, the normalizations have been recalculated using our RM samples.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Constraints on the mean and dispersion of the distribution of individual f factors based on the line dispersion measured from the rms spectrum, using a sample of 30 objects with dynamical-modeling and RM BH masses as compiled in Table 3. Top: raw distribution of individual f factors. The ML estimates of the sample mean and intrinsic 1σ dispersion are marked. Bottom: Marginalized probability distributions of the mean and intrinsic 1σ dispersion of f factors. The 16%, peak, and 84% locations of the distributions are marked.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Comparisons between M RM from two lines for the same object. For Mg II, we have corrected the rms line dispersion for the velocity split V ≈ 750 km s−1 of the doublet (﹩{\sigma }_{\mathrm{true}}=\sqrt{{\sigma }_{\mathrm{measure}}^{2}-{(V/2)}^{2}}﹩). There is general agreement between the RM masses measured from two different lines, validating the RM technique of measuring BH masses. The two most significant outliers in the line comparisons are marked with their RMIDs.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Comparisons of the detected lags between two different methods (ICCF vs. PyROA at left and Javelin vs. PyROA at right). In most cases, our fiducial PyROA lags are consistent with the ICCF lags. However, for our multiyear light-curve data, the Javelin method often traps the lag in the seasonal gaps, leading to artificial clustering of lags there.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Lag detection fraction as a function of line variability parameter SNR2, for Hβ, Mg II, and C IV, respectively. Error bars are Poisson counting uncertainties.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Comparisons between lags from two different lines for the same object. Hα and Mg II lags are typically longer than Hβ lags, while C IV lags are somewhat shorter (but the sample statistics are limited, and the scatter is large) than Mg II lags.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: Key Results
Authors: Yue Shen, Catherine J. Grier, Keith Horne, Zachary Stone, Jennifer I. Li, Qian Yang, Yasaman Homayouni, Jonathan R. Trump, Scott F. Anderson, W. N. Brandt, Patrick B. Hall, Luis C. Ho, Linhua Jiang, Patrick Petitjean, Donald P. Schneider, Charling Tao, Fergus. R. Donnan, Yusra AlSayyad, Matthew A. Bershady, Michael R. Blanton, Dmitry Bizyaev, Kevin Bundy, Yuguang Chen, Megan C. Davis, Kyle Dawson, Xiaohui Fan, Jenny E. Greene, Hannes Gröller, Yucheng Guo, Héctor Ibarra-Medel, Yuanzhe Jiang, Ryan P. Keenan, Juna A. Kollmeier, Cassandra Lejoly, Zefeng Li, Axel de la Macorra, Maxwell Moe, Jundan Nie, Graziano Rossi, Paul S. Smith, Wei Leong Tee, Anne-Marie Weijmans, Jiachuan Xu, Minghao Yue, Xu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Redshift distribution of RM masses derived from Hα, Hβ, Mg II, and C IV lags for the SDSS-RM sample. Error bars are measurement uncertainties only and do not include the ∼0.3 dex systematic uncertainty in M RM.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: The relation between β obs and f esc,LyC, f esc,LyC ξ ion. The gray circles represent LyC leakers at z ∼ 0.3 from Chisholm et al. (2022), where β obs are measured as observed stellar continuum slope at 1550 Å. The gray downward arrows refer to the 1σ upper limits of f esc,LyC for galaxies without LyC detected, i.e., LyC flux is not significantly detected given the observed backgrounds. The gray dashed line and the shaded region are the analytical relations of f esc,LyC and f esc,LyC ξ ion with respect to β obs, and the 1σ uncertainties of the relations. The orange stars are our stack f esc,Lyα  measurements assuming the Calz dust law, scaled by a factor of 0.15 according to Begley et al. (2023), and the orange dashed lines are the best-fit f esc,Lyα −β obs and f esc,Lyα  ξ ion−β obs relation as described in Equation (9), also scaled by 0.15.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption:  f esc,Lyα  ξ ion as a function of β obs, M UV,att, and M ⋆ assuming the Calz dust law. The blue circles indicate f esc,Lyα  ξ ion for each individual LAEs, and purple triangles are f esc,Lyα  ξ ion of non-LAEs with forced measured f esc,Lyα . The fringed orange stars indicate the stack f esc,Lyα  ξ ion for all HAEs. We adopt the stack f esc,Lyα  values and the median ξ ion of HAEs in each stack bin. We show the best-fit relations between the stack f esc,Lyα  ξ ion of all HAEs and β obs, M UV,att, M ⋆ as the orange lines. In the left panel, we show the scaled f esc,LyC ξ ion−β obs relations, which is the f esc,LyC ξ ion−β obs relation in Chisholm et al. (2022) divided by 0.15, as the gray dashed line.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: The redshift evolution of global f esc,Lyα  from z = 0 to z = 8. Our stacked measurement of f esc,Lyα  for all HAE samples is shown as a red diamond based on the assumption of Calz dust law. The orange and white diamonds are f esc,Lyα  measured by stacking the HAE sample in two redshift bins (z = 5.24, 5.84). f esc,Lyα  measurements compiled by Hayes et al. (2011) based on Lyα and UV (z > 2.2) or Hα luminosity densities (z < 2.2) are shown in blue circles, and the best-fit relation for their compilation is shown as the blue dashed line. The green circles denote the measurements in Konno et al. (2016), also using Lyα and UV LFs, and their best-fit relation is shown as the green dashed line. The purple squares are the f esc,Lyα  derived from Lyα and Hα luminosity densities at z > 5 in Sun et al. (2023) with HAEs observed by NIRCam/WFSS.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption:                       ﹩{f}_{\mathrm{esc},\mathrm{Ly}\alpha }^{\mathrm{rel}}﹩                      ξ ion as a function of M UV,att, and M ⋆ assuming the Calz dust law. The blue circles indicate ﹩{f}_{\mathrm{esc},\mathrm{Ly}\alpha }^{\mathrm{rel}}﹩                      ξ ion for each individual LAEs, and purple triangles are ﹩{f}_{\mathrm{esc},\mathrm{Ly}\alpha }^{\mathrm{rel}}﹩                      ξ ion of non-LAEs with forced measured ﹩{f}_{\mathrm{esc},\mathrm{Ly}\alpha }^{\mathrm{rel}}﹩. The fringed orange stars indicate the stack ﹩{f}_{\mathrm{esc},\mathrm{Ly}\alpha }^{\mathrm{rel}}﹩                      ξ ion for all HAEs. We adopt the median stack f esc,Lyα  values and the median ξ ion and A UV of HAEs in each stack bin. We show the best-fit relations of the stack f esc,Lyα  ξ ion of all HAEs with respect to M UV,att, M ⋆ as the orange lines.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: The coupling of β obs and E(B − V) on the dependence of f esc,Lyα  on M ⋆, M UV,att, M UV,att, ξ ion, sSFR, and ΣsSFR. We show the f esc,Lyα  of individual LAEs as circles and forced measured f esc,Lyα  of non-LAEs as triangles, color-coded by their β obs. The stack f esc,Lyα  are marked as stars color-coded by the median β obs in each stack bin. The solid and dashed lines are predicted f esc,Lyα  from Equation (9) based on the median β obs and E(B − V) in each stack bin, respectively.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: The flux distribution of selected HAEs (left panel) and color–color diagrams showing our photometric selection criteria (middle and right panel). The magenta dots represent the Hα flux and magnitude of our HAE sample. In the left panel, we label the typical uncertainty in line flux and magnitude. Overlying colored dots are emitters from JAGUAR mocks, residing in redshift windows that their specific emission lines could be captured by F444W grism: Hα at z ≈ 4.9–6.7, [O III]λ5007 at z ≈ 6.9–9.0, He I at z ≈ 2.5–3.6, Paα λ10830 at z ≈ 1.05–1.7, and [S III] λ9532 at z ≈ 3.0–4.3. Our selection criteria matches well with mock HAEs and can effectively rule out most low-redshift objects.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: The accumulative emissivity of galaxies at z = 5.5. Here, ﹩\tfrac{{\dot{n}}_{\mathrm{ion}}(\gt {M}_{\mathrm{UV}})}{{\dot{n}}_{\mathrm{ion},\ \mathrm{tot}}}﹩ refers to the fraction of ionizing budget contributed by galaxies fainter than a specific M UV,att, as in Equation (13). We set the faint-end limit ﹩{M}_{\mathrm{lim}}=-13﹩ and −10 for ﹩{\dot{n}}_{\mathrm{ion},\mathrm{tot}}﹩, shown as the red and blue lines respectively. We mark M UV,att = − 16 as the vertical dotted line for reference.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: The two double-peaked Lyα-emitting galaxies in our final HAE sample. For each source, we show the 1.″25 × 1.″25 red, green, and blue thumbnail in the right panel, composed of JWST F182M, F210M, and F444W. The left panels show the rest-frame Lyα spectra extracted from the MUSE cubes.
Paper: Quantifying the Escape of Lyα at z ≈ 5–6: A Census of Lyα Escape Fraction with Hα-emitting Galaxies Spectroscopically Confirmed by JWST and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Yunjing Wu, Zihao Li, Fengwu Sun, Xiaohui Fan, Zuyi Chen, Mingyu Li, Fuyan Bian, Yuanhang Ning, Linhua Jiang, Gustavo Bruzual, Stephane Charlot, Jacopo Chevallard
Figure caption: Same as Figure 6 while assuming the SMC dust attenuation law. The dashed lines and gray-shaded regions represent the best-fit analytical relation as described in Equation (9).