adsabs/AstroCLIMB huggingface dataset:
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: The redshift distribution (yellow) of ASPIRE quasars used in this work, in the ascending order of redshift, and the redshift range of the Lyα forest used in the analysis is denoted by the red horizontal line. We exclude the Lyα forest spectrum at >1176 Å rest frame to exclude the possible emission from the quasar proximity zone and exclude the rest λ < 1040 Å Lyα forest to exclude the contamination from O VI λ 1033 emission and the Lyβ forest. The redshift range of ASPIRE quasars used in this work is from z ∼ 6.5 to z ∼ 6.8 and the corresponding Lyα absorption redshift range is from z ∼ 5.4 up to z ∼ 6.6.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: The first and the third rows show the CDFs of the τ eff around [O III] emitters at 5.4 < z < 6.1 (yellow-green), adopting influence radii from 5 h −1 cMpc to 50 h −1 cMpc. The random cumulative distribution function of the τ eff around [O III] emitters is shown in brown, representing the τ eff distribution of IGM patches. The optimistic and the pessimistic CDFs are plotted in dashed and dotted lines, respectively. The second and the fourth rows show the fitted CDFs from the KM estimator and the 1σ confidence interval of the CDF is shown in the shaded regions of the corresponding color. The null hypothesis p-value from the log-rank test is shown in the bottom right corner of each subpanel. See the text for more details.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Top—The stacked transmission of the Lyα forest around [O III] emitters (red) and away from [O III] emitters (blue), adopting the inverse variance weighting and an influence radius of 25 h −1 cMpc; see the text for details. Middle—The stacked transmission of the Lyα forest around [O III] emitters (red) and away from [O III] emitters (blue), where the stacked transmission is the unweighted average transmission. Bottom—The number of quasar LOSs available in each pixel of the stacked Lyα forest transmission around [O III] emitters (red) and the stacked Lyα forest transmission away from [O III] emitters (blue).
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Similar to Figure 10, but for [O III] emitters at 5.4 < z < 5.7.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: The τ eff measurements of the stacked Lyα forest spectrum centered at [O III] emitters (the red line in the top panel of Figure 6) are denoted by red open squares, and the τ eff measurements of the stacked Lyα forest spectrum away from [O III] emitters (the blue line in the top panel of Figure 6) are marked by blue open hexagons. Individual measurements of IGM optical depth around [O III] emitters τ eff,[O III] are shown in filled gray squares, adopting an influence radius of 25 h −1 cMpc. The best-fit redshift evolutions of τ eff from J. Yang et al. (2020b) and S. E. I. Bosman et al. (2022) are denoted by the orange and the purple lines, respectively.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: (a) The distribution of τ eff around the [O III] emitters (τ eff,[O III]) by adopting an influence radius of 25 h −1 cMpc. (b) The random distribution of τ eff,[O III] by adopting an influence radius of 25 h −1 cMpc. The distributions of 2σ lower limits of τ eff are shown in red in (a) and (b). (c) The CDFs of the τ eff,[O III] (yellow-green) and the random distribution (brown). For 2σ lower limits of τ eff, we plot them as actual measurements (solid line) or infinity (dashed line) in CDF.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Similar to Figure 9, but for [O III] emitters at 5.7 < z < 6.1.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: The transmitted spectrum of all quasars used in this work, in the ascending order of R.A. The transmitted spectrum (black) has been smoothed with a median filter for better visualization. The spectral uncertainty is shown in gray. The redshift range of the Lyα used in the analysis is displayed in the red-shaded region. The location of the Lyβ emission line is marked by the blue downward arrow. The spatial locations of the [O III] emitters identified in each quasar field are denoted by the yellow-green circles in terms of the [O III] emitter redshift z [O III] and the transverse distance r ⊥ between the [O III] emitter and the central quasar.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Average transmitted flux around [O III] emitters (filled yellow-green stars), weighted by the integrated length of each τ eff,[O III] measurement, as a function of influence radii at 5.4 < z < 6.1, 5.7 < z < 6.1, and 5.4 < z < 5.7. The 1σ uncertainty is calculated using bootstrapping. The random values are denoted by filled brown stars.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: (continued.) The transmitted spectrum of ASPIRE quasars J0244+5008, J0305−3150, J0525−2406, and J1048−0109, together with [O III] emitters detected in the quasar fields.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: The first and the third rows show the CDFs of the random τ eff around [O III] emitters (brown) and τ eff of IGM patches (black) at 5.4 < z < 6.1. The influence radius is from 5 h −1 cMpc to 50 h −1 cMpc for τ eff,[O III] measurements and τ eff are measured using the bin size of twice the corresponding influence radius. The optimistic and the pessimistic CDFs are plotted in dashed and dotted lines, respectively. The second and the fourth rows show the fitted CDFs from the KM estimator and the 1σ confidence interval of the CDF is shown in the shaded regions of the corresponding color. The null hypothesis p-value from the log-rank test is shown in the bottom right corner of each subpanel. With all influence radii, the random τ eff,[O III] distribution is consistent with the τ eff distribution of IGM patches.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: The CDF of the random τ eff,[O III] (brown) and τ eff of IGM patches (black) at 5.4 < z < 5.7.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: The CDF of the random τ eff,[O III] (brown) and τ eff of IGM patches (black) at 5.7 < z < 6.1.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Growth rates of unstable modes with nonzero background pressure gradients, as a function of wavenumbers. Left: AdSI-dominant case (﹩\widetilde{\eta }=0.005﹩). Right: classical SI-dominant case (﹩\widetilde{\eta }=0.05﹩).
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Linear growth rates of the AdSI as a function of ϵ and α M for fixed St = 0.1, obtained from Equation (12); see M.-K. Lin & C.-Y. Hsu (2022).
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: (continued.) The LOS plot of ASPIRE quasars J2102−1458 and J2232+2930, together with [O III] emitters detected in the quasar fields.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: (continued.) The LOS plot of ASPIRE quasars J1104+2134, J1129+1846, J1526−2050, and J2002−3013, together with [O III] emitters detected in the quasar fields.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Spacetime plot of dusty filaments with ϵ = 1. We compute the vertical average density at every time to show the evolution of filaments within our simulation timescale. From left to right the panels show the cases with α M = 100, 10−1, 10−2, and 10−3 respectively.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Evolution of dust-density perturbation of the fiducial case. Panels correspond to different initial α M. We use different colors to indicate different initial ϵ, and we also show the clumping condition in the plot (dashed–dotted line).
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Same as Figure 4 but with α M equals to 1, 0.01, and 0.001 from left to right panels. Note that for the red line in the middle panel, the AdSI saturates at negligible amplitudes and thus appears stable. This is the same as the red and yellow lines in the right panel.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Snapshots of dust density of α M = 0.1. The time is set to be t = 100P, when the disks are in a quasisteady state. From top to bottom panels, the cases with ϵ = 102, 101, 100, 10−1, and 10−2 are indicated respectively.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Overview of the end state with different initial α M and ϵ in our simulations. The red curve delineates the critical dust-to-gas ratio ϵ crit(α M) as the function of α M. Cases above this curve meet the clumping condition. We also include the relevant simulations from (HL22; in blue symbols) for comparison.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Evolution plot of dust-density growth normalized by initial density in α M = 0.1. The color shows different initial ϵ, which is the same as Figure 4.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Same as Figure 6 but with α M = 0.01.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Similar to Figure 9 but for α M = 0.1 and St = 0.01.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Evolution of dust density normalized by initial dust. Color lines indicate disks with different initial grain sizes.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Similar to Figure 9 but with ﹩\widetilde{\eta }=0.05﹩ and varying α M. Left: pure classical SI and α M = 0 (dark-red line in Figure 12). Right: classical SI with some background accretion flow α M = 0.1 (dark-green line in Figure 12).
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Evolution of maximum dust density with different box sizes. We compare the simulation box in this study (red line) with the box 2 and 4 times the length along each side. The left and right panels show the changing box size in a radial and vertical direction. The number of cells is chosen to keep the resolution per H g constant.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Similar to Figure 4 but for disk with radial pressure gradient ﹩\widetilde{\eta }=0.05﹩. In three cases (dark-red, orange, and dark-green lines), we set the initial α M = 0.1.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Similar to Figure 4 but in terms of the maximum dust-density perturbation ﹩\delta {\rho }_{{\rm{d}},\max }=\max ({\rho }_{{\rm{d}}}-\epsilon {\rho }_{0})﹩.
Paper: Streaming Instabilities in Accreting Protoplanetary Disks: A Parameter Study
Authors: Shiang-Chih Wang, Min-Kai Lin
Figure caption: Dust and gas density perturbation of fiducial case at t = 100 P. Both dust and gas density strength are normalized by initial density.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Left: predicted neutrino spectra of GRB 090902B for the dissipative photosphere model with R ph = 1.1 × 1012 cm, Γ = 580, and ε  p /ε  e  = 3. Three lines are corresponding to different values of f  p , e.g., solid line (f  p  = 1.0), dashed line (f  p  = 0.5), and dotted line (f  p  = 0.3). Right: constraint on ε  p /ε  e  of GRB 090902B within dissipative photosphere model for R ph = 1.1 × 1012 cm and Γ = 580. The solid black and blue lines are N sig = 1 at δ ≈ 27.°9 by adopting the effective areas of IC59 and IC86II, respectively.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Left: predicted neutrino spectra of GRB 230307A for the ICMART model with R ICMART = 1016 cm, Γ = 300, and ε  p /ε  e  = 3. Three lines are corresponding to different values of f  p , e.g., solid line (f  p  = 1.0), dashed line (f  p  = 0.5), and dotted line (f  p  = 0.3). The gray line with arrows is the upper limit of time-integrated muon-neutrino flux for IceCube (IceCube Collaboration 2023). Right: constraint on ε  p /ε  e  of GRB 230307A for the ICMART model with R ICMART = 1016 cm and Γ = 300.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Left: predicted neutrino spectra of GRB 211211A for the dissipative photosphere model with R ph = 1010 cm, Γ = 200, and ε  p /ε  e  = 3. Three lines are corresponding to different values of f  p , e.g., solid line (f  p  = 1.0), dashed line (f  p  = 0.5), and dotted line (f  p  = 0.3). Right: constraint on ε  p /ε  e  of GRB 211211A within dissipative photosphere model for R ph = 1010 cm and Γ = 200.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Left: predicted neutrino spectra of GRB 080916C for the ICMART model with R ICMART = 1016 cm, Γ = 500, and ε  p /ε  e  = 3. Three lines are corresponding to different values of f  p , e.g., solid line (f  p  = 1.0), dashed line (f  p  = 0.5), and dotted line (f  p  = 0.3). Right: constraint on ε  p /ε  e  of GRB 080916C for the ICMART model with R ICMART = 1016 cm and Γ = 500. The solid black and blue lines are N sig = 1 at δ ≈ −56.°6 by adopting the effective areas of IC40 and IC86II, respectively.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Left: expected number of neutrino signal events for a GRB 211211A-like event as a function of the luminosity distance. The horizontal dotted line is N sig = 1. Right: probability of detecting more than one neutrino associated with a GRB 211211A-like event as a function of the luminosity distance. The vertical dotted lines are d  L  = 40 Mpc and d  L  = 300 Mpc. The solid and dashed lines are corresponding to adopt the effective area of IceCube and IceCube-Gen2 for different declinations, respectively. f  p  = 0.3 and ε  p /ε  e  = 3 are adopted.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Model-independent constraint on the R–Γ diagram for GRB 211211A. The lines represent N sig = 1 with different GRB parameters, e.g., the solid red line (ε  p /ε  e  = 10 and f  p  = 1); the solid black line (ε  p /ε  e  = 3 and f  p  = 1); the dotted black line (ε  p /ε  e  = 3 and f  p  = 0.5).
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Left: IC86II effective area as a function of the neutrino energy with different declinations for IceCube. Right: The effective area of other periods used (e.g., IC40 and IC59) in this paper is taken from IceCube Collaboration et al. (2021).
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage. II. Results of Four Seasons of Observation
Authors: Hai-Cheng Feng, Sha-Sha Li, J. M. Bai, H. T. Liu, Kai-Xing Lu, Yu-Xuan Pang, Mouyuan Sun, Jian-Guo Wang, Yang-Wei Zhang, Shuying Zhou
Figure caption: Long-term light curve of NGC 4151. Data from different bands were intercalibrated using PyCALI, with ASAS-SN g-band data as the reference.