adsabs/AstroCLIMB huggingface dataset:
Paper: Cross-survey Image Transformation: Enhancing SDSS and DECaLS Images to Near-HSC Quality for Advanced Astronomical Analysis
Authors: Zhijian Luo, Shaohua Zhang, Jianzhen Chen, Zhu Chen, Liping Fu, Hubing Xiao, Wei Du, Chenggang Shu
Figure caption: Example images of three groups of galaxies. The panels, arranged from left to right, showcase images of different galaxies, while those arranged from bottom to top correspond to the observations of the same galaxy from three surveys with varying depths and resolutions: HSC, DECaLS, and SDSS. The images used are sourced from publicly available data on the official Legacy Survey website.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Display to illustrate and compare the distributions of StOB spacings for 17 targets in Table 5 having ≥2 StOBs with measured spacings. Open circles are continuous StOBs and filled symbols are for StOBs having intervals of quiescence between StOBs. (Only FY Per and CM Del have extended multiyear trains of continuous StOBs. The remainder of the “open-circle“ targets in this figure have only occasional shorter fragments of continuous StOBs, and the spacings used in the figure are taken from these fragments.) Each line is a separate target, and the targets are arranged bottom-to-top in order of increasing mean spacing. An abbreviated name of each target appears on the right. Some data points have been adjusted slightly in position to minimize overlaps, but this does not affect the properties of the distributions. An X Ser point at spacing = 161 days falls off the plot, as indicated by the arrow on line 17. The vertical scale is arbitrary, used to space the systems vertically such that overlap is minimized.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Mean amplitude of StOBs in each target against orbital period. The pair of vertical dashed lines marks the period gap between 2.15 and 3.12 hr (from C. Knigge 2011). See the text for details (Section 6.2). The outlier V426 Oph is marked.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Seasonal averages for BK Lyn. Large solid points are seasons with NL behavior. Open circles are seasons with DN behavior. Small solid points are seasons with a likely mixture of NL and DN, designated NL+. These designations are aligned with the relevant clusters of points on the bottom line of the plot. Error bars are standard deviation of a single observation, or the rms. The averages and the error bars for NL+ are for the restricted magnitude range V = 14.74–14.34. See the text for details.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Outburst amplitude vs. time for X Ser, over ∼23 yr. Averages over ∼5 yr intervals are also shown, with error bars corresponding to the standard deviation of the mean. Fifteen points are from Table 5, three points are for MMO StOBs not in Table 5 (because they have too few measured parameters), but which appear in the seasonal plots, and five points are from V. Šimon (2018).
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Like Figure 9, except to illustrate and compare the distributions of the StOB amplitudes for 29 targets in Table 5 having ≥3 StOBs with measured amplitudes. Each line is a separate target, and the targets are arranged bottom-to-top in order of increasing mean amplitude. An abbreviated name of each target appears on the right. An X Ser point at amplitude = 2.63 mag (StOB #15 in Table 5 falls off the plot.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Rise time of StOB against decline time, for the faster StOBs. This is an expanded portion of Figure 11. Note that, in a majority of the systems, the average rise is faster than the average fall. See the text for details (Section 6.2).
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Sequences on three nights in 2011–12 for MV Leo (=1H 1025+220). Data points spaced closer that 15 mag are connected by straight lines. See Table 4 for details on these sequences.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Average of the fall times of StOBs for each target against average of the decline times, expressed as the e-folding time, τ, in days. The outlier RW Sex is labeled. See the text for details (Section 6.2).
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Mean amplitude of StOBs in each target against average of rise and fall times. See the text for details (Section 6.2).
Paper: Extracting Cleaned Swift/UVOT Ultraviolet Grism Spectra with the uvotpy Package
Authors: Hao Zhou, Stefano Covino, Zhi-Ping Jin, Yi-Zhong Fan, Da-Ming Wei, N. Paul Kuin
Figure caption: The 2D UV nominal spectrum of AG+81 266. The red region represents the trace of the optimal/default extraction aperture spanning from 1700 to 5000 Å. Upper and lower background regions are shown by dashed red lines above and below the central spectrum, respectively. From pixel number (PN) ∼50 (i.e., ∼2800 Å), the second-order spectrum becomes visible, and begins to overlap with the extraction aperture. Because AG+81 266 is bright and blue enough, the third-order spectrum is also visible starting from PN ∼450. Both the second- and the third-order wavelengths at the PN where the first-order wavelength is 5000 Å (i.e., in this figure, the PN ∼ 660), are less than 2600 Å. Hence, the contamination can be removed with the first-order spectrum free of the contamination (λ < 2600 Å).
Paper: Extracting Cleaned Swift/UVOT Ultraviolet Grism Spectra with the uvotpy Package
Authors: Hao Zhou, Stefano Covino, Zhi-Ping Jin, Yi-Zhong Fan, Da-Ming Wei, N. Paul Kuin
Figure caption: Cleaned first-order spectra of the four white dwarfs used to calibrate the second-order effective area. The black lines represent clean first-order spectra, and the gray dashed lines represent the raw first-order spectra extracted with uvotpy. Reference spectra are shown with red dotted–dashed lines. The bin width is 25 Å. For GD 153, the spectrum suffers from the strong coincidence loss from ∼3000 Å to ∼4000 Å, hence the intensity of the clean spectrum is a bit lower than the reference value. For WD 1657+343, the signal-to-noise ratio is too low for λ ≳ 3800 Å, and the uncertainty is quite large, which is not plotted. Generally, the second-order contamination is removed from the raw spectra, and the third-order contamination for λ ≲ 4500 Å is negligible even for β ∼ −1.5.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Comparison of outbursts and standstills of Z Cam stars (open and filled circles) with OBs and SS-like features in StOB stars (crosses). The vertical axis is equivalent to ΔSS (see Section 8). Filled circles are data from the Z Cam light curves in M. Simonsen et al. (2014) while open circles are from the Z Cam systems observed at the MMO (see Tables 10, 13, and 14). The MMO Z Cam stars duplicate (in identity) many of the M. Simonsen et al. (2014) stars, but the data differ in both years observed and in technique (CCD employed for MMO data and a mixture of CCDs and visual for the M. Simonsen et al. 2014 data). Note that in this particular characterization of light curves, the OBs and SSs in StOB stars (crosses) appear as an extension to the trends of Z Cam stars (circles).
Paper: Extracting Cleaned Swift/UVOT Ultraviolet Grism Spectra with the uvotpy Package
Authors: Hao Zhou, Stefano Covino, Zhi-Ping Jin, Yi-Zhong Fan, Da-Ming Wei, N. Paul Kuin
Figure caption: The effective area of the second-order spectrum when using the default/optimal extraction aperture. The thin blue line represents the built-in effective area in the uvotpy package with the first-order anchor position of (1080, 1000) in detector pixels, and the thick orange line is derived with spectra listed in Table 1 with the mean anchor position of (988.4, 1080.2). Both shaded regions represent the 1σ uncertainty.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Average of rise/fall times of StOBs against FWHM. See the text for details (Section 6.2). The outlier RW Sex is marked.
Paper: Extracting Cleaned Swift/UVOT Ultraviolet Grism Spectra with the uvotpy Package
Authors: Hao Zhou, Stefano Covino, Zhi-Ping Jin, Yi-Zhong Fan, Da-Ming Wei, N. Paul Kuin
Figure caption: First-order anchor positions of spectra listed in Table 1. Different markers represent different targets, excepting the black cross, which represents the mean first anchor position of the all spectra used to calibrate the second-order effective area.
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Amplitude of photometric dips against amplitudes of accompanying StOBs. The dashed line corresponds to 1:1 behavior. See the text for details (Section 5).
Paper: Stunted Outbursts and Z Cam–like Behaviors in the Long-term Light Curves of Novalike Cataclysmic Variables
Authors: R. K. Honeycutt, Jeff W. Robertson, Brandon T. Radzom
Figure caption: Widths of photometric dips against widths of accompanying StOBs. See the text for details (Section 5).
Paper: Collision-energy-sensitive State Selectivity and Line Ratios in Charge Exchange between N5+ and He
Authors: X. B. Zhu, R. T. Zhang, C. J. Zhang, S. Mitrani, L. Gu, Y. Gao, S. F. Zhang, X. Ma
Figure caption: (a)–(c) The fractions of the ℓ-resolved state-selective population for n = 3 capture in CX between N5+ ions and He atoms. The present measurements (navy blue squares), the measurements from P. H. Cotte et al. (1985; brown diamonds), the calculated results from M. C. Bacchus-Montabonel & K. Amezian (1990; pink line), the measurements from (D. Dijkkamp et al. 1985; blue circles), with the different line formats (blue lines, green dotted lines, red dotted lines, and purple dotted lines) representing the results calculated by the statistical, separable, LZ, and even, respectively.
Paper: Collision-energy-sensitive State Selectivity and Line Ratios in Charge Exchange between N5+ and He
Authors: X. B. Zhu, R. T. Zhang, C. J. Zhang, S. Mitrani, L. Gu, Y. Gao, S. F. Zhang, X. Ma
Figure caption: The measured Q spectra of single CX between N5+ ions and He atoms. The incident projectile energies are 5.36, 10.71, 17.5, 25, 32, 38, 45, 64, and 75 keV u−1, from top to bottom and column by column. Circles show the present measurement, and red and blue vertical lines show the 2ℓ state-selective capture and the target excitation, respectively. Blue dashed lines mark the Gaussian curve fitting and red dashed lines mark the sum of the Gaussian fitting results.
Paper: Collision-energy-sensitive State Selectivity and Line Ratios in Charge Exchange between N5+ and He
Authors: X. B. Zhu, R. T. Zhang, C. J. Zhang, S. Mitrani, L. Gu, Y. Gao, S. F. Zhang, X. Ma
Figure caption: (a) The experimentally derived UV emission following CX between 5.36 keV u−1 N5+ ions and He atoms. The FWHM is set as 0.5 eV for visibility. (b) The line ratios dependence on the collision energy. I3p→2s / I3d→2p: the present measurements (red circles), the measurements from P. H. Cotte et al. (1985; red squares), the measurements from D. Dijkkamp et al. (1985; red triangles). I3s→2p/I3d→2p: the present measurements (black circles), the measurements from P. H. Cotte et al. (1985; black squares), the measurements from D. Dijkkamp et al. (1985; black triangles).
Paper: Collision-energy-sensitive State Selectivity and Line Ratios in Charge Exchange between N5+ and He
Authors: X. B. Zhu, R. T. Zhang, C. J. Zhang, S. Mitrani, L. Gu, Y. Gao, S. F. Zhang, X. Ma
Figure caption: Relative cross sections of n-resolved state-selective CX process for N5+ ion collisions with He atoms. The present measurements are : n = 2 (black circles); n = 3 (red circles); n = 4 (blue triangles); n = 5 (purple diamonds); and n ≥ 6 (brown squares).
Paper: Collision-energy-sensitive State Selectivity and Line Ratios in Charge Exchange between N5+ and He
Authors: X. B. Zhu, R. T. Zhang, C. J. Zhang, S. Mitrani, L. Gu, Y. Gao, S. F. Zhang, X. Ma
Figure caption: The longitudinal recoil-ion momentum P∥ vs. the transverse recoil-ion momentum P⊥ for n- and ℓ- resolved state-selective CX between 25 keV u−1 N5+ ions and quasi-stationary He atoms.
Paper: Collision-energy-sensitive State Selectivity and Line Ratios in Charge Exchange between N5+ and He
Authors: X. B. Zhu, R. T. Zhang, C. J. Zhang, S. Mitrani, L. Gu, Y. Gao, S. F. Zhang, X. Ma
Figure caption: The collision energy dependence of the ratios between state-selective CX cross sections of σ2p and σ2s in N5+ ion collisions with He atoms.
Paper: SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
Authors: Hiroya Umeda, Masami Ouchi, Satoshi Kikuta, Yuichi Harikane, Yoshiaki Ono, Takatoshi Shibuya, Akio K. Inoue, Kazuhiro Shimasaku, Yongming Liang, Akinori Matsumoto, Shun Saito, Haruka Kusakabe, Yuta Kageura, Minami Nakane
Figure caption: Redshift evolution of xH I. The red circles (squares) and bars represent our xH I estimates and uncertainties based on the Lyα LFs (LAE clusterings), respectively. Besides the xH I estimates from this work, we also present xH I estimates from literature using Lyα LFs (circles; M. Ouchi et al. 2010; A. Konno et al. 2014; Z.-Y. Zheng et al. 2017; A. K. Inoue et al. 2018; H. Goto et al. 2021; A. M. Morales et al. 2021; Y. Ning et al. 2022; I. G. B. Wold et al. 2022), LAE clustering (squares; E. Sobacchi & A. Mesinger 2015; M. Ouchi et al. 2018), Lyα damping wing measurements of LBGs (diamonds; E. Curtis-Lake et al. 2023; T. Y.-Y. Hsiao et al. 2024; H. Umeda et al. 2024), damping wing measurements of QSOs (right-tipped triangles; J. Schroeder et al. 2013; F. B. Davies et al. 2018; B. Greig et al. 2019; F. Wang et al. 2020; D. Ďurovčíková et al. 2024), damping wing measurements of GRBs (left-tipped triangles; T. Totani et al. 2006, 2014), Lyα equivalent width distributions (X marks; A. Mesinger et al. 2015; A. Hoag et al. 2019; C. A. Mason et al. 2019; I. Jung et al. 2020; L. R. Whitler et al. 2020; P. Bolan et al. 2022; S. Bruton et al. 2023; T. Morishita et al. 2023; M. Nakane et al. 2024; M. Tang et al. 2024; G. C. Jones et al. 2025), Lyα forests and/or Lyα + β dark fraction/gap measurements (pluses; X. Fan et al. 2006; A. Mesinger et al. 2015; Y. Zhu et al. 2022, 2024; X. Jin et al. 2023; B. Spina et al. 2024), and the electron scattering of the CMB (pentagon; Planck Collaboration et al. 2020). The pink symbols represent estimates based on JWST data (E. Curtis-Lake et al. 2023; T. Morishita et al. 2023; T. Y.-Y. Hsiao et al. 2024; M. Nakane et al. 2024; M. Tang et al. 2024; H. Umeda et al. 2024; G. C. Jones et al. 2025).
Paper: SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
Authors: Hiroya Umeda, Masami Ouchi, Satoshi Kikuta, Yuichi Harikane, Yoshiaki Ono, Takatoshi Shibuya, Akio K. Inoue, Kazuhiro Shimasaku, Yongming Liang, Akinori Matsumoto, Shun Saito, Haruka Kusakabe, Yuta Kageura, Minami Nakane
Figure caption: Redshift evolution of the bias of LAEs as a function of redshift. The red circles represent the average galaxy bias of our LAEs at z = 2.2, 3.3, 4.9, 5.7, and 6.6. The black and white circles are the LAE bias values from M. Ouchi et al. (2018) and M. Ouchi et al. (2010), respectively. The black and white stars represent LAE bias values obtained by M. Ouchi et al. (2005b) and M. Ouchi et al. (2003), respectively. The black and white squares are the LAE bias values measured by L. Guaita et al. (2010) and R. S. Kovač et al. (2007), respectively. The black and white diamonds represent the LAE bias measured by E. Gawiser et al. (2007) and H. Kusakabe et al. (2018), respectively. All the bias measurements are corrected to match the σ8 value consistent with Planck Collaboration et al. (2020). The solid lines indicate the bias of the dark matter halos with a halo mass of 108, 109, 1010, 1011, and 1012M⊙ when each dark matter halo hosts one galaxy (M. Ouchi et al. 2018). The dotted lines represent the redshift evolution of bias in the case of a galaxy-conserving model (J. N. Fry 1996).
Paper: SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
Authors: Hiroya Umeda, Masami Ouchi, Satoshi Kikuta, Yuichi Harikane, Yoshiaki Ono, Takatoshi Shibuya, Akio K. Inoue, Kazuhiro Shimasaku, Yongming Liang, Akinori Matsumoto, Shun Saito, Haruka Kusakabe, Yuta Kageura, Minami Nakane
Figure caption: (Left) Redshift evolution of Lyα and dust-attenuated UV luminosity densities. The red circles and bars represent the Lyα luminosity densities and the uncertainties derived by integrating the fitted DPL function down to the Lyα luminosity of Lcut/erg s−1 = 42.5. The blue circles and bars represent the UV luminosity densities from R. J. Bouwens et al. (2022) derived by integrating down to the UV luminosity of MUV = −17.0 mag. The red and blue shading corresponds to the uncertainty ranges for the Lyα and UV luminosity densities across the redshifts, respectively. (Right) Zoomed-in view of the redshift evolution of the Lyα and UV luminosity densities at the EoR. The solid red (blue) line represents the best-fit ∝(1 + z)ξ function with ξ as a free parameter fitted by the Lyα (UV) luminosity densities at z = 5.7−7 (z = 6−8). The dashed lines are the extrapolation of the fitted ∝(1 + z)ξ functions.
Paper: SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
Authors: Hiroya Umeda, Masami Ouchi, Satoshi Kikuta, Yuichi Harikane, Yoshiaki Ono, Takatoshi Shibuya, Akio K. Inoue, Kazuhiro Shimasaku, Yongming Liang, Akinori Matsumoto, Shun Saito, Haruka Kusakabe, Yuta Kageura, Minami Nakane
Figure caption: e-folding scale of Lyα equivalent width distribution at different redshifts. Our EW0,e constraints derived from the distribution fitting between 40 and 200 (1000) Å data are shown as red filled (blue unfilled) circles. EW0,e values from L. Napolitano et al. (2024) and L. Pentericci et al. (2018) are shown as red stars and pentagons, respectively. EW0,e values from J. Kerutt et al. (2022) and T. Shibuya et al. (2018b) are shown as a blue hexagon and blue stars, respectively. We also present values from L. L. Cowie et al. (2010), R. Ciardullo et al. (2012), K. K. Nilsson et al. (2009), N. Kashikawa et al. (2011), E. M. Hu et al. (2010), and Z. Zheng & J. Wallace (2014) as a black x mark, white squares, black squares, black diamonds, white diamonds, and a black pentagon, respectively.
Paper: SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
Authors: Hiroya Umeda, Masami Ouchi, Satoshi Kikuta, Yuichi Harikane, Yoshiaki Ono, Takatoshi Shibuya, Akio K. Inoue, Kazuhiro Shimasaku, Yongming Liang, Akinori Matsumoto, Shun Saito, Haruka Kusakabe, Yuta Kageura, Minami Nakane
Figure caption: Comparison between cosmic reionization scenarios and xH I estimates. The solid, dotted, and dashed lines and shading represent xH I evolution predictions from S. L. Finkelstein et al. (2019), M. Ishigaki et al. (2018), and R. P. Naidu et al. (2020), respectively. The red circles and squares represent xH I from this work based on Lyα LFs and LAE clusterings, respectively. The red diamonds and x marks represent the xH I estimates from the LBG damping wing by H. Umeda et al. (2024) and those from Lyα equivalent width distributions by M. Nakane et al. (2024), respectively.
Paper: SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
Authors: Hiroya Umeda, Masami Ouchi, Satoshi Kikuta, Yuichi Harikane, Yoshiaki Ono, Takatoshi Shibuya, Akio K. Inoue, Kazuhiro Shimasaku, Yongming Liang, Akinori Matsumoto, Shun Saito, Haruka Kusakabe, Yuta Kageura, Minami Nakane
Figure caption: Comparison between observed LAEs’ two-point ACFs and predictions by our 21CMFAST simulations at z = 4.9, 5.7, and 6.6 for different xH I. The black dots and the bars represent the observed ACFs and their errors used for xH I inference, respectively. On the left panel, we show the predicted ACF and 68th percentile uncertainty at xH I = 0 at z = 4.9 as a dashed line and gray shading, respectively. For the other redshifts, we show the ACF at xH I = 0.0, 0.2, 0.4, 0.6, and 0.8. The ACF monotonically increases with xH I increase.
Paper: SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
Authors: Hiroya Umeda, Masami Ouchi, Satoshi Kikuta, Yuichi Harikane, Yoshiaki Ono, Takatoshi Shibuya, Akio K. Inoue, Kazuhiro Shimasaku, Yongming Liang, Akinori Matsumoto, Shun Saito, Haruka Kusakabe, Yuta Kageura, Minami Nakane
Figure caption: Comparison between observed Lyα LFs and predictions by our 21CMFAST simulations at z = 4.9, 5.7, 6.6, 7.0, and 7.3 for different xH I. The black dots and the bars represent the observed LFs and their errors, respectively. On the upper left panel, we show the predicted LF and 68th percentile uncertainty at xH I = 0 at z = 4.9 as a dashed line and gray shading, respectively. For the other redshifts, we show the LF at xH  = 0.0, 0.2, 0.4, 0.6,  and 0.8. The LF monotonically decreases with xH I increases. We show the 68th percentile uncertainty for the LFs at xH I = 0.0 as references.