adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: Normalized 1σ errors on the circumbinary-planet parameters as a function of the planetary period P for BNS and DWD sources observed by B-DECIGO and DECIGO. The curves show the error on K and on P, each rescaled by the GW SNR and by Mp (in MJ), so that lower values indicate tighter constraints. Errors remain small when multiple orbital cycles are sampled, develop a minimum at intermediate P (where the Doppler imprint strengthens), and then rise sharply once P approaches or exceeds the mission duration; a feature near P ∼ 1 yr reflects degeneracy with the detector’s annual motion. Default source and observing assumptions are used throughout.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: DECIGO: same as Figure 7 but for an extragalactic case at DL = 1 Gpc. Even at cosmological distances, high-Mc, near-equal-mass binaries allow detection of giant planets with ﹩{M}_{p}^{{\rm{\min }}}﹩ of a few Jupiter masses under the adopted criterion and mission duration.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: Selection function in the plane of planetary mass versus orbital separation for CBPs around compact binaries. The solid curves give, for each detector and source class (BNS/DWD), the minimum detectable mass ﹩{M}_{p}^{{\rm{\min }}}﹩ at a given orbital distance a, adopting the detection criterion σK/K < 0.3 and σP/P < 0.3. The horizontal dashed line marks the deuterium-burning limit at 13 MJ. DECIGO outperforms B-DECIGO across the board, and BNS hosts yield substantially lower ﹩{M}_{p}^{{\rm{\min }}}﹩ than DWDs due to their higher carrier GW frequencies.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: Minimum detectable planetary mass ﹩{M}_{p}^{{\rm{\min }}}﹩ versus luminosity distance DL for equal-mass BNS reference systems, comparing B-DECIGO (3 yr) and DECIGO (4 yr). As DL increases, the SNR drops and ﹩{M}_{p}^{{\rm{\min }}}﹩ rises; DECIGO’s lower noise floor and longer integration push the sensitivity from super-Earth/Neptune scales in the Galaxy to sub-Jovian levels well beyond, under the same 30% detection criterion on (K, P).
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: Detector sensitivity adopted in this work. We show the characteristic noise ﹩{h}_{n}(f)\equiv \sqrt{f\,{S}_{n}(f)}﹩ for B-DECIGO and DECIGO. The two overlaid source tracks indicate the premerger signal strength of the reference compact binaries (BNS and DWD), and the vertical lines mark the GW frequencies reached 100 yr before coalescence.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: Source-frame coordinates ﹩({\hat{x}}^{{\prime} },\ {\hat{y}}^{{\prime} },\ {\hat{z}}^{{\prime} })﹩; detector-frame coordinates ﹩(\hat{x},\ \hat{y},\ \hat{z})﹩; and ecliptic coordinates ﹩(\bar{x},\ \bar{y},\ \bar{z})﹩.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: Illustration of a three-body system composed of a BNS and a CBP.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Simulated light curves for the e = 0.7 model (M05e07b). Each colored curve shows the isotropic-equivalent bolometric luminosity from various viewing directions as defined in Figure 1. Dashed curves show the light curve from intermediate viewing angles θ = π/4 (45° off the orbital plane) of the corresponding directions. The gray curve shows the accretion luminosity from the NS particle (Equation (11)) and the black crosses are the observed light curve of SN2022jli (P. Chen et al. 2024). The brown shaded region covers the phase where we expect the main SN ejecta to be optically thick, and thus, our accretion-powered light curve is still not visible (see Section 4.2).
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Profiles of density, pressure, temperature, opacity, and radial velocity as a function of distance from the companion core. Each curve corresponds to the density profile along a specific radial ray and is colored according to the latitudinal angle. The brown vertical lines mark the location of the NS. We choose a snapshot from model M05e08b_r at t = 50 days, which is the fourth periastron. The gray dashed curves show the initial profiles. The overlaid red solid curve is an example ejecta density profile of a type Ic SN.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Same as Figure 13 but for t = 56.25 days, the fifth apastron.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Time evolution of the mass ejected from the donor star. We compare all models with M2 = 5 M⊙. We treat model M05e05b as the “Baseline” model and color variations are the same as in Figures 4, 6, and 7.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Upper panel: effective temperature from our light-curve simulations for various viewing directions. Lower panel: photospheric radius computed from the simulations. Colors of the curves indicate the same viewing directions as in Figure 9.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Same as Figure 4 but comparing the optimistic (model M05e07b; red) versus realistic (model M05e07b_r; purple, M05e08b_r; dark brown) models for the mass accretion rate.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Same as Figure 4 but comparing models with different eccentricities: e = 0.3 (model M05e03b; pink), 0.5 (model M05e05b; dark gray), and 0.7 (model M05e07b; red). All models were simulated with bipolar feedback.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Same as Figure 10 but for the realistic mass accretion model.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Same as Figure 11 but for the realistic mass accretion model.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Subtracting the average radial trend from the processed coronagraph image. (a) A polarized brightness image obtained from STEREO COR1 coronagraph on 2017 August 25 (see Section 3.2 for details). (b) The azimuthally averaged radial trend Itr(r) (Equation (1)). (c) The two-dimensional trend array ﹩{I}_{\mathrm{tr}}\left(\sqrt{{(x-{x}_{0})}^{2}+{(y-{y}_{0})}^{2}}\right)﹩. (d) The detrended image ﹩{I}_{\mathrm{detr}}﹩. The dynamic ranges of the original (a) and the detrended (d) images are saturated at 95% percentile levels for better clarity. The images are plotted in the relative coordinates X = x − x0, Y = y − y0.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: QRaFT segmentation of the central-plane density array in the MAS model. (a) Processed image array ﹩{I}_{\mathrm{detr}}﹩ (3) in Cartesian coordinates after radial detrending and smoothing; (b) transformed array I(ϕ, ρ) (4) in plane polar coordinates; (c) the signed second-order azimuthal difference array Idiff (6); (d) the unsigned second-order difference array Ienh (7) after azimuthal detrending; (e) tracing unsigned second-order azimuthal gradients, with the colors marking 10 tracing runs with different inner boundary ﹩{\rho }^{{\rm{\min }}}﹩; (f) final tracing product obtained by combining the individual tracing runs and automatically removing unreliable features as explained in Section 2.5.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Misalignment angle statistics describing the discrepancy between the QRaFT features detected in the central-plane density array (top) and in the synthetic pB image (bottom) obtained from the MAS model, as compared to the POS orientation of the magnetic field in the same model. (a) The occurrence rate histogram of the signed angle misalignment θB angle; (b) the occurrence rate histogram of the unsigned angle ∣θB∣; (c) normalized cumulative distribution on the unsigned angle, showing occurrence rates for three characteristic percentile levels. The parameters μ, m, and σ in panels (a)–(b) are respectively the sample mean, the median, and the standard deviation of the corresponding sample.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Top panels: automatic validation of the QRaFT features detected in the central-plane density (left) and pB brightness (right) outputs of the MAS model. Red lines show the validated features that meet the filtering conditions (25)–(31) and are included in the final data product; blue lines show the discarded features excluded from the final QRaFT product. The processed enhanced images are shown in the background. Bottom panels: validated QRaFT features traced in the density array (left) and the synthetic pB image (right) obtained from the MAS model overplotted with the POS magnetic field lines (brown) in the same model.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Segmenting simulated quasi-radial coronal structures using unsigned second-order azimuthal differencing. Left column: a simple model of an azimuthal intensity profile represented by a single Gaussian function. Right column: a more complex model composed of several randomly generated Gaussian peaks. Panels (a) and (e): processed intensity profiles; panels (b) and (f): first-order azimuthal differences; panels (c) and (g): signed (black) and unsigned (red) second-order azimuthal differences; panels (d) and (h): simulated POS intensity variability corresponding to the studied profiles. Red dashed vertical lines show local maxima of the unsigned second-order difference (shown with diamonds on panels (c) and (g)). These lines are aligned with the large-scale density gradients, which are expected to be constrained by the coronal magnetic field, enabling an image-based field-line tracing.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: QRaFT segmentation of a synthetic pB image produced by MAS and FORWARD codes. See Figure 5 for notations.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Explanation of the geometric parameters of pixel clusters detected by QRaFT. The number assigned to each pixel represents the label λ of the cluster to which it belongs, as well as the subscript of its metrics defined in Section 2.4. R is the set of the radial positions involved in the cluster (12), Φ(ρ) is the two-level set of the azimuthal positions corresponding to each ρ (11), δρ is the radial extent of the cluster (17), δϕ is the azimuthal thickness of the cluster (16), and s is the discrete area of the cluster (18).
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Misalignment angle statistics for the QRaFT features detected in the COR1 image. Notations are the same as in Figure 8.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: QRaFT segmentation of a COR1 pB image aligned with the synthetic MAS images shown in Section 3.1. See Figure 5 for notations.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Schematic diagram showing the angular metrics (21)–(24) at the location of a selected feature node. See text for details.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: (Top) Stellar mass vs. SFR plot for our final sample of 94 emitters. The colors of the data points are the same as those in Figure 5, with orange triangles representing narrowband selected emitters and gray circles representing those confirmed with spectroscopic redshifts. The SFRs are calculated based on the Hα emission line flux after removing the [N II] contribution and correcting for dust extinction. Error bars are propagated from uncertainties in the Hα flux and extinction, derived from the Hα/Hβ ratio. The cyan line indicates the star-forming main sequence at z = 0.9 from P. Popesso et al. (2023), and the black dashed line marks 0.1 times the main sequence level. (Bottom) Same as the top panel but for the subsample with IRAC coverage, where the rest-frame UVJ diagram is used to classify quiescent galaxies.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Clustocentric radius versus physical properties of galaxies for cluster A (left) and group G (right). Symbols for star-forming and sub-main-sequence galaxies are consistent with those defined in Figure 7. The Spearman rank correlation coefficients (ρs) and associated p-values for both the full population and the star-forming subsample are indicated within each panel.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Stellar mass vs. extinction diagram. Blue hexagons represent star-forming galaxies, while small red hexagons denote sub-main-sequence galaxies, defined as those lying more than 0.3 dex below the star-forming main sequence. Black crosses mark spectroscopically confirmed emitters with filter response corrections applied to both Hα and Hβ fluxes. The orange and indigo lines represent the Hα/Hβ ratios as a function of stellar mass derived from the HST WISP survey (0.75 ≤ z ≤ 1.5; A. Domínguez et al. 2013) and the Keck MOSDEF survey (z ∼ 2.3; A. E. Shapley et al. 2022), respectively. The shaded regions around these lines indicate the corresponding uncertainties. The dashed line indicates the intrinsic Hα/Hβ ratio in the dust-free case under the Case B recombination assumption.
Paper: Electron Instabilities Driven by Beaming Electrons with Anisotropic Temperatures in High-beta Plasmas
Authors: Ye Yu, Jinsong Zhao, Chen Shi, Huasheng Xie
Figure caption: The scenario of the electron instability in the two-dimensional parameter space of Veb/VA and Aeb = Teb⊥/Teb∥. (a) The maximum growth rate γ normalized by the electron cyclotron frequency ωce; (b) the normalized real frequency ωr/ωce; (c) the wave-normal angle θ; and (d) the wave polarization defined as ﹩P=-{\rm{Im}}\left(\frac{{B}_{x}{B}_{y}^{* }}{| {B}_{x}| | {B}_{y}| }\right)\times {\rm{sign}}({\omega }_{r})﹩. The five instability regimes are labeled as “I,” “II,” “III,” “IV,” and “V” in (a).
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Rest-frame UVJ diagram used to classify galaxy populations; colors are derived from SED fitting including Subaru and IRAC observations as described in Section 4.1. The orange solid lines represent the quiescent galaxy boundaries defined in Z. Mao et al. (2022). Blue filled circles represent star-forming galaxies, and red filled circles represent quiescent galaxies identified by the UVJ diagram.
Paper: Electron Instabilities Driven by Beaming Electrons with Anisotropic Temperatures in High-beta Plasmas
Authors: Ye Yu, Jinsong Zhao, Chen Shi, Huasheng Xie
Figure caption: The electron instabilities in the isotropic temperature case. The distributions of the normalized maximum growth rate γ/ωce (a), the normalized real frequency ωr/ωce (b), and the polarization P (c) in the Veb–θ parameter space. The distributions of γ/ωce (d), ωr/ωce (e), and P (f) in the Veb–k parameter space. The three vertical dashed lines denote the boundaries among the instability Regimes I, II, and III.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Cumulative distribution functions and p-value derived from the KS test comparing galaxies in cluster A (overdense regions) and the rest of the fields (moderate-density regions).
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Color–magnitude diagram for selected emission-line galaxies across all six fields. Orange data points indicate galaxies in cluster A (overdense regions), while blue data points represent galaxies in the remaining fields (moderate-density regions).
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Top left: cosmic ionizing emissivity as a function of the redshift, ﹩{\dot{n}}_{{\rm{ion}}}(z)﹩, from stars only and assuming primordial metallicity, Z = 10−4. The blue-filled region shows minimum/maximum bounds by considering fesc = 1%/100% with the lighter blue showing the 1σ uncertainty of the CSFH fit propagated through. Top right: same as the top left, only for solar metallicity, Z = 0.02. Bottom left: neutral fraction as per Equation (3) for primordial metallicity. The filled regions have the same meaning as the top panels. The gold star with the horizontal error bar shows the midpoint and 1σ uncertainty of reionization inferred from Planck Collaboration (2020a). Bottom right: same as the bottom left, but for solar metallicity.