adsabs/AstroCLIMB huggingface dataset:
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Means and relative standard deviations of the fitted P (top), and relative deviations and standard deviations of the fitted τ (bottom) as functions of the temporal resolutions, where the mean and relative standard deviation of the fitted p, or the relative deviation and relative standard deviation of the fitted τ are marked by the plus sign and rhombus, with their corresponding linear fitting results represented by three blue lines.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Deviations between the statistical averages of forward simulation’s fitted τ and their standard τ as cataloged by A. Nechaeva et al. (2019), where the relative deviations are plotted as a function of the standard τ, and their statistical distribution are presented in the bottom panel.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: The ratio of the relative standard deviations of the fitted p to τ is plotted as a function of the model τ/p, where the ratio reported in the catalog is shown in the top panel, and the ratio obtained from forward simulations is presented in the bottom panel.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Means and standard deviations of the fitted P (top) and τ (bottom) as functions of c2, where the mean and standard deviation are marked by the plus sign and rhombus, respectively.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Deviations in τ between forward simulations and their standard models are plotted as a function of their corresponding model periods (top) and amplitudes (bottom).
Paper: Fourier and Wavelet Analysis of Coronal Mass Ejections during Solar Cycles 23–25: Angular Widths and Latitudinal Distribution
Authors: Wenhua Wang, Zuo Jiang, Linhua Deng, Jinlei Li, Xuewen Tan, Jie Cao, Tingting Xu, Miao Wan, Weihong Zhou
Figure caption: The first column presents the Fourier spectra, and the second column shows the method for estimating the significance of Fourier spectral power peaks. The third column depicts the global wavelet spectra, and the fourth column illustrates the local wavelet spectra for different angular widths of daily CMEs. In the Fourier spectra, the dashed red lines indicate the 95% confidence level. The second column shows the logarithm of cumulative probability vs. power for actual daily CME counts and a randomized sequence. In the global wavelet spectra, the dashed red lines represent the 95% confidence level against the red-noise background. Statistically significant regions in the local wavelet spectra, at the 95% confidence level relative to the red-noise background, are contoured by thick black lines. From top to bottom, the rows represent all high-latitude and low-latitude CMEs, spanning the period from 1996 January to 2024 March.
Paper: Fourier and Wavelet Analysis of Coronal Mass Ejections during Solar Cycles 23–25: Angular Widths and Latitudinal Distribution
Authors: Wenhua Wang, Zuo Jiang, Linhua Deng, Jinlei Li, Xuewen Tan, Jie Cao, Tingting Xu, Miao Wan, Weihong Zhou
Figure caption: The analysis of halo CMEs from 1996 January to 2024 March. The figure displays Fourier spectra (first column), a schematic for estimating the significance of Fourier spectral power peaks (second column), global wavelet spectra (third column), and local wavelet spectra (fourth column).
Paper: Fourier and Wavelet Analysis of Coronal Mass Ejections during Solar Cycles 23–25: Angular Widths and Latitudinal Distribution
Authors: Wenhua Wang, Zuo Jiang, Linhua Deng, Jinlei Li, Xuewen Tan, Jie Cao, Tingting Xu, Miao Wan, Weihong Zhou
Figure caption: Global wavelet spectra and local wavelet spectra for different angular widths of daily northern CMEs for SC23 (the first column), SC24 (the second column), and SC25 (the third column). From top to bottom, each unit contains two rows, the first row shows high-latitude CMEs and the second row shows low-latitude CMEs. Each unit represents narrow CME, normal CME, and halo CME respectively.
Paper: Fourier and Wavelet Analysis of Coronal Mass Ejections during Solar Cycles 23–25: Angular Widths and Latitudinal Distribution
Authors: Wenhua Wang, Zuo Jiang, Linhua Deng, Jinlei Li, Xuewen Tan, Jie Cao, Tingting Xu, Miao Wan, Weihong Zhou
Figure caption: The analysis of narrow CMEs from 1996 January to 2024 March. The figure displays Fourier spectra (first column), a schematic for estimating the significance of Fourier spectral power peaks (second column), global wavelet spectra (third column), and local wavelet spectra (fourth column).
Paper: Fourier and Wavelet Analysis of Coronal Mass Ejections during Solar Cycles 23–25: Angular Widths and Latitudinal Distribution
Authors: Wenhua Wang, Zuo Jiang, Linhua Deng, Jinlei Li, Xuewen Tan, Jie Cao, Tingting Xu, Miao Wan, Weihong Zhou
Figure caption: The analysis of normal CMEs from 1996 January to 2024 March. The figure displays Fourier spectra (first column), a schematic for estimating the significance of Fourier spectral power peaks (second column), global wavelet spectra (third column), and local wavelet spectra (fourth column).
Paper: Fourier and Wavelet Analysis of Coronal Mass Ejections during Solar Cycles 23–25: Angular Widths and Latitudinal Distribution
Authors: Wenhua Wang, Zuo Jiang, Linhua Deng, Jinlei Li, Xuewen Tan, Jie Cao, Tingting Xu, Miao Wan, Weihong Zhou
Figure caption: Wavelet spectra for different angular widths of daily northern CMEs for SC23 (the first column), SC24 (the second column), and SC25 (the third column). From top to bottom, the first row shows all high-latitude CMEs and the second row shows all low-latitude CMEs.
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 cleaned first-order spectrum of GRB 130427A. The gray and black lines are the raw first-order spectrum extracted with uvotpy and the cleaned first-order spectrum. The bin width is 100 Å. Red points represent photometries obtained by the RAPTOR-T telescope. The blue dashed line is the power-law function with β = 0.8. The RAPTOR-T ﹩{g}^{{\prime} }﹩-band photometry matches the cleaned spectrum well, which implies the third-order contamination is negligible for 4000 Å ≲ λ ≲ 5000 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: The deviation of cleaned first-order spectra from reference spectra and the statistical 1σ uncertainty. The bin width of the wavelength is 100 Å, and the deviation is defined as the quotient of the residuals between cleaned spectra and reference spectra divided by the reference spectra. For λ < 2800 Å, the spectrum is free of contamination. The median absolute deviation and the uncertainty are ∼0.8% and ∼3.7%, respectively. For 2800 Å < λ < 4000 Å, the spectrum only suffers from the second-order contamination and the median values are ∼1.3% and ∼11.2%, respectively. For λ > 4000 Å, except the second-order contamination, the spectrum also suffers from the third-order contamination, hence the deviation roughly keeps becoming larger (especially for ≳4500 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: The cleaned first-order spectrum of 3C 273. The raw and cleaned spectra are shown with the gray and black lines respectively, and the bin width of the wavelength is 25 Å. The reference spectrum shown with the red line is taken by HST/STIS on 1999 January 31, and to match the intensity of UVOT UV grism spectrum, the reference spectrum is multiplied by a factor of 1.6. The blue dashed line is the power-law function with β = 0.5. The higher-order contamination begins to dominate at λ ∼ 5100 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: The logarithm of CR2/CR1 to base 10 for different spectral indices (y-axis) at a specified wavelength (x-axis). The black lines represent contours and the numbers in the black lines represent values of the contours. For 3600 Å < λ < 4000 Å, the second-order count rate is greater than 10% of the first-order count rate when β < 2.
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: The fitting result for the Lyα LF at z = 7.3. The circles and squares with bars represent the number densities and corresponding error bars from this work and A. Konno et al. (2014), respectively. These filled symbols are used to fit the Lyα LFs. The lines and shading represent the same statistics described in Figure 7.
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: Two-point angular autocorrelation function ω(θ) of LAEs at z = 2.2, 3.3, 4.9, 5.7, and 6.6. Black circles with bars represent the observed correlation functions and errors. The solid and dashed lines represent the best-fit power-law model in and outside of the fitting range used, respectively. The dotted–dashed line represents the correlation function of the dark matter density fluctuation ωDM(θ) at each redshift. The vertical dotted lines represent the boundary for angular scales used for the fitting.
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: Evolution of Lyα LF after the epoch of cosmic reionization. The Lyα LFs for z = 4.9, 5.7, 6.6, 7.0, and 7.3 are shown in pale blue, yellow, orange, pink, and red, respectively. The solid (dashed) lines represent the median of the fitted DPL (Schechter) functions in the luminosity range used in the fitting. The shading represents the 68th percentile range for the fitted functions at the redshift of corresponding color. The symbols in each color represent the same parameters depicted in Figures 7, 8, 9, 10, and 11, 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: Evolution of Lyα LF after the epoch of cosmic reionization. The Lyα LFs for z = 2.2, 3.3, and 4.9 are shown in purple, blue, and pale blue, respectively. The solid (dashed) lines represent the median of the fitted DPL + DPL (Schechter + DPL) functions in the luminosity range used in the fitting. The shading represents the 68th percentile range for the fitted functions at the redshift of corresponding color. The symbols in each color represent the same parameters depicted in Figures 5, 6, and 7, 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: The 2D marginalized PDFs for ﹩\mathrm{log}{\phi }_{{\rm{gal}}}^{\star }﹩ and ﹩\mathrm{log}{\phi }_{{\rm{agn}}}^{\star }﹩ when DPL functions are fitted for the galaxy and AGN components. The purple, blue, and pale blue contours represent the 2D marginalized PDFs for the Lyα LF at z = 2.2, 3.3, and 4.9, respectively. The dark and light components for each contour represent the 68th and 90th percentile ranges, respectively. Note that the PDFs for z = 3.3 and 4.9 reach the lower-bound values for the ﹩\mathrm{log}{\phi }_{{\rm{agn}}}^{\star }﹩ prior (i.e., ﹩\mathrm{log}{\phi }_{{\rm{agn}}}^{\star }/{{\rm{cMpc}}}^{-3}=1{0}^{-10}﹩).
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: The 2D marginalized PDFs for ﹩\mathrm{log}{\phi }_{{\rm{gal}}}^{\star }﹩ and ﹩\mathrm{log}{L}_{{\rm{gal}}}^{\star }﹩ when the Schechter (DPL) function is fitted for the galaxy (AGN) component. The purple, blue, and pale blue contours represent the 2D marginalized PDFs for the Lyα LF at z = 2.2, 3.3, and 4.9, respectively. The dark and light components for each contour represent the 68th and 90th percentile ranges, 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: The fitting result for the Lyα LF at z = 6.6. The circles, squares, upward triangles, diamonds, stars, pentagons, and downward triangles with bars represent the number densities and corresponding error bars from this work, M. Ouchi et al. (2010), A. Konno et al. (2018), S. Santos et al. (2016), A. J. Taylor et al. (2021), J. Matthee et al. (2015), and Y. Ning et al. (2022), respectively. Filled (open) symbols are used (not used) to fit the Lyα LFs. The lines and shading represent the same statistics described in Figure 7.
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: The 2D marginalized PDFs for ﹩\mathrm{log}{\phi }^{\star }﹩ and ﹩\mathrm{log}{L}^{\star }﹩ when the Schechter function is fitted. The pale blue, yellow, orange, pink, and red contours represent the 2D marginalized PDFs for the Lyα LF at z = 4.9, 5.7, 6.6, 7.0, and 7.3, respectively. The dark and light components for each contour represent the 68th and 90th percentile ranges, 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: The fitting result for the Lyα LF at z = 7.0. The circles, squares, upward triangles, diamonds, stars, and pentagons with bars represent the number densities and corresponding error bars from this work, K. Ota et al. (2017), R. Itoh et al. (2018), Z.-Y. Zheng et al. (2017), W. Hu et al. (2019), and I. G. B. Wold et al. (2022), respectively. Filled (open) symbols are used (not used) to fit the Lyα LFs. The lines and shading represent the same statistics described in Figure 7.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: Top-left panel: the distribution of line width of the blueshifted/redshifted [O III] components (σb/σr). Top-middle panel: the distribution of the line flux ratio (Fb/Fr). Top-right panel: the relationship between peak separations and redshifts. Bottom-left panel: the relationship between Vb/Vr and Fb/Fr. Bottom-middle panel: the relationship between Vb and σb. Bottom-right panel: the relationship between Vr and σr.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: The best-fitting results of the emission lines around Hα. In the top of each panel, the solid dark green line shows the line spectrum after subtracting starlight (if present) from the host galaxy with Plate-Mjd-Fiberid shown in the top-left corner. The solid red line represents the best-fitting results with χ2/dof shown in the top-left corner, the dashed cyan line represents continuum emission, the solid green lines represent the determined components of the broad Hα emission line, the dashed green line represents the narrow Hα emission line, the solid blue lines represent the [O I] emission lines (if present), and the dashed purple lines represent the [N II] and [S II] doublets. In the bottom of each panel, the solid blue line represents the residuals calculated by the line spectrum minus the best-fitting results and then divided by the uncertainties of the SDSS spectrum. The horizontal solid and dashed green lines show residuals = 0,  ±1, respectively.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: The best-fitting results of the emission lines around double-peaked narrow Hα emission lines. In the top of each panel, the solid dark green line shows the line spectrum after subtracting starlight (if present) determined from host galaxy with Plate-Mjd-Fiberid shown in the top-left corner, the solid red line represents the best-fitting results with χ2/dof shown in the top-left corner, the dashed cyan line represents continuum emission, the dashed purple lines represent the [N II] and [S II] doublets, the solid green lines represent the broad Hα emission line, and the dashed blue line and red line represent the blueshifted and redshifted components of the narrow Hα, respectively. In the bottom of each panel, the solid blue line represents the residuals calculated by the line spectrum minus the best-fitting results and then divided by the uncertainties of the SDSS spectrum. The horizontal solid and dashed green lines show residuals = 0, ±1, respectively.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: The SDSS spectra of the 62 type 1 AGNs in the final sample. In each panel, the solid dark green line represents the spectrum with Plate-Mjd-Fiberid shown in the top-left corner, the solid red line shows the best-fitting results with χ2/dof (if present) shown in the top-left corner, the solid blue line shows starlight (if present), the solid green line represents the AGN continuum emission, and the solid black line represents the line spectrum calculated by the SDSS spectrum minus the best-fitting results (if present).
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: An example of the offsets of [O III] and narrow Hα emission lines is the object with single-peaked narrow Hα emission lines in our sample in velocity space. The solid blue line represents the determined blueshifted component of [O III], and the vertical blue line marks the position of the central wavelength of the blueshifted component of [O III], the solid red line represents the determined redshifted component of [O III], and the vertical red line marks the position of the central wavelength of the redshifted component of [O III], the solid green line shows the determined narrow Hα component, and the vertical green line marks the position of the central wavelength of the narrow Hα.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: Distributions of redshift (left panel), black hole masses MBH (right panel) for the 558 typical type 1 AGNs from Y. Shen et al. (2011b) (histogram filled with blue line), and the 62 type 1 AGNs with double-peaked [O III] in our sample (histogram filled with red lines).
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: Photometric image properties of the seven type 1 AGNs with double-peaked [O III].
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 results of transforming DECaLS images to HSC images using the Pix2WGAN model. The images display three different galaxies from left to right, with the original DECaLS images shown at the top, the model-generated pseudo-HSC images in the middle, and the corresponding actual HSC observational images at the bottom.
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: Schematic diagram of the classical pix2pix network architecture. xlow represents the low-quality input image, xenhanced represents the enhanced image generated by the generator after transformation, and xhigh represents the high-quality target/real image. G is the generator, which adopts a U-Net structure, while D is the discriminator, whose task is to distinguish between the authenticity of the input image pairs.