adsabs/AstroCLIMB huggingface dataset:
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 [O III]. In the top of each panel, the solid dark green line shows the line spectrum after subtracting starlight (if present) determined from the host galaxy with Plate-Mjd-Fiberid shown in the top-left corner. The solid red line represents the best-fitting results with two narrow Gaussian functions describing each core component of the [O III] doublet, and the corresponding ﹩{\chi }_{1}^{2}/{{\rm{dof}}}_{1}﹩ is shown in the top-left corner. The ﹩{\chi }_{2}^{2}/{{\rm{dof}}}_{2}﹩ determined by one narrow Gaussian function for each core component of the [O III] doublet is shown in the top-left corner. The dashed cyan line represents continuum emission, the solid purple lines represent Fe II emission lines, the solid green lines represent broad Hβ emission lines, the solid cyan lines represent the extended component of [O III], and the dashed blue and red lines represent the blueshifted and the redshifted components of [O III], 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 offsets of [O III] and narrow Hα emission lines for the 53 objects with the single-peaked narrow Hα emission lines in our sample in velocity space. In each panel, 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: Production and Loss Processes of Hydrogen Energetic Neutral Atoms in the Heliosphere from 5 eV–500 keV
Authors: Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak
Figure caption: Left column: the collision rates for the ENA loss processes in the heliospheric condition sets defined in Table 1 (color solid and dashed lines) and the combined collision rate (black dotted line). Right column: the ENA loss exposure factors for ENAs traversing the SSW, FSW, heliosheath, and VLISM regions (panels top to bottom). The line colors and styles are the same, as shown in Figure 4. The colors of shaded areas correspond to IMAP ENA detector energy ranges, as in Figure 2.
Paper: Production and Loss Processes of Hydrogen Energetic Neutral Atoms in the Heliosphere from 5 eV–500 keV
Authors: Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak
Figure caption: Reaction rate coefficient for the electron impact ionization of hydrogen ENAs. The left and middle panels show the results of the numerical integration with the Maxwellian distribution, and the approximation given in Equations (6)–(7), respectively. The right panel presents the difference between the calculated rate coefficients using these two approaches. The red lines in the left and middle panels mark the reaction rate coefficient of 10−9 cm3 s−1.
Paper: Production and Loss Processes of Hydrogen Energetic Neutral Atoms in the Heliosphere from 5 eV–500 keV
Authors: Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak
Figure caption: Cross sections for ENA loss processes discussed in Section 5 (except photoionization) as a function of the collision energy. The cross sections for the charge exchange and ionization losses in collisions with the same species are marked with solid and dashed lines of the same color.
Paper: Production and Loss Processes of Hydrogen Energetic Neutral Atoms in the Heliosphere from 5 eV–500 keV
Authors: Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak
Figure caption: Left column: the collision rates for the ENA production processes in the heliospheric condition sets defined in Table 1 (colored lines) and the combined production rate (black dotted line). Right column: the relative contributions of individual processes to the combined collision rate. The shaded areas correspond to the energy ranges of the IMAP ENA instruments: IMAP-Lo (orange), IMAP-Hi (cyan), and IMAP-Ultra (magenta). Note the energy ranges overlap between the instruments.
Paper: Production and Loss Processes of Hydrogen Energetic Neutral Atoms in the Heliosphere from 5 eV–500 keV
Authors: Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak
Figure caption: Comparison of the cross sections for the production of hydrogen ENAs. The cross sections are obtained from the formulae discussed in this paper; see Table 2 for references.
Paper: Production and Loss Processes of Hydrogen Energetic Neutral Atoms in the Heliosphere from 5 eV–500 keV
Authors: Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak
Figure caption: Comparison of the proton–hydrogen atom charge exchange cross sections considered in this study. The top panel compares the absolute cross sections. The middle and bottom panels show ratios to the recommended formula given in Equation (A1) and from P. Swaczyna et al. (2019b), respectively.
Paper: Production and Loss Processes of Hydrogen Energetic Neutral Atoms in the Heliosphere from 5 eV–500 keV
Authors: Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak
Figure caption: Comparison of the recommended cross section values from N. D. Cariatore & D. R. Schultz (2021) with the obtained fit formula and the cross section reproduced using the Chebyshev polynomial coefficients from C. F. Barnett (1990; reaction E-2).
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: Similar to Figure 3. This figure presents three additional examples of transformation results from DECaLS images to HSC images using the Pix2WGAN model.
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 SDSS images to HSC images using the Cascade Pix2WGAN model. The images display the same three galaxies as in Figure 3, with the original SDSS 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: Similar to Figure 8. The images display the same three galaxies as in Figure 4, with the original SDSS 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: Architecture of the Cascade Pix2WGAN Model. G1 and G2 represent the generators, while D1 and D2 represent the discriminators. XSDSS, XDECaLS, and XHSC denote the real observational images obtained from SDSS, DECaLS, and HSC, respectively. Meanwhile, ﹩{\widetilde{{\rm{X}}}}_{{\rm{DECaLS}}}﹩ and ﹩{\widetilde{{\rm{X}}}}_{{\rm{HSC}}}﹩ represent the pseudo-DECaLS and pseudo-HSC images generated by the model, respectively.
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: Similar to Figure 3. This figure shows galaxy images where the actual HSC observational images exhibit significant streak-like artifacts (left column), prominent noise (middle column), or partial overexposure (right column). In contrast, the model-transformed pseudo-HSC images successfully remove the artifacts, reduce noise interference, and correct the overexposure.
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: Similar to Figure 3. In these galaxy images, the actual DECaLS observational images exhibit significant streak-like artifacts (left column), significant noise (middle column), or blurriness (right column), while the model-transformed pseudo-HSC images successfully remove the artifacts, reduce noise interference, and improve overall image clarity.
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 daily occurrence rate of all CMEs from 1996 January to 2024 March, with daily rates represented on the left vertical axis, corresponding to the line plot, and monthly rates on the right vertical axis, corresponding to the bar plot. Panel (a) illustrates the occurrence rates of all CMEs across the full solar disk. Panel (b) presents the occurrence rates for high-latitude CMEs (orange-shaded region), while panel (c) depicts the occurrence rates for low-latitude CMEs (purple-shaded region). The red dashed lines mark the transition points between successive solar cycles.
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 daily occurrence rate of halo CMEs from 1996 January to 2024 March. Panel (a) shows the occurrence rates across the full solar disk. Panel (b) presents the rates for high-latitude halo CMEs (orange regions), while panel (c) displays the rates for low-latitude halo CMEs (purple regions). The red dashed lines indicate the transitions between solar cycles.
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 daily occurrence rate of normal CMEs from 1996 January to 2024 March. Panel (a) shows the occurrence rates across the full solar disk. Panel (b) presents the rates for high-latitude normal CMEs (orange regions), while panel (c) displays the rates for low-latitude normal CMEs (purple regions). The red dashed lines indicate the transitions between solar cycles.
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 daily occurrence rate of narrow CMEs from 1996 January to 2024 March. Panel (a) shows the occurrence rates across the full solar disk. Panel (b) presents the rates for high-latitude narrow CMEs (orange regions), while panel (c) displays the rates for low-latitude narrow CMEs (purple regions). The red dashed lines indicate the transitions between solar cycles.
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: Schematic synthetic light curves for six types of StOBs. See Sections 5 and 6.3 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: Four examples of StOB/dip pairs. All are Type 2 StOBs except RW Sex, which is Type 3. The JD axis is JD-2448000. See Section 5 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: Histogram of the separations (in days) of ∼150,000 MMO light-curve points. See the text for details (Section 3.3).
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 LFs of this work at z = 2.2, 3.3, 4.9, 5.7, 6.6, 7.0, and 7.3. The red filled circles and bars represent the number densities and their errors at each redshift using the data from all survey fields. The black squares, left-tipped triangles, diamonds, stars, pentagons, and right-tipped triangles represent the number density calculated for the UD-COSMOS, D-COSMOS, UD-SXDS, D-SXDS, D-DEEP23, and D-ELAISN1 fields, respectively. The red open circles with upper-side arrows represent the number density and the lower limit based on the spectroscopically identified sources in our photometric sample. The spectroscopic confirmation of objects in our photometric LAE samples is based on M. Ouchi et al. (2008, 2010, 2025, in preparation), S. J. Lilly et al. (2009), A. L. Coil et al. (2011), R. P. Mallery et al. (2012), D. Masters et al. (2012), O. Le Fèvre et al. (2013), T. Shibuya et al. (2014, 2018a, 2018b), M. Kriek et al. (2015), J. Liske et al. (2015), D. Sobral et al. (2015), I. G. Momcheva et al. (2016), W. Hu et al. (2017), L. Jiang et al. (2017, 2018), L. A. M. Tasca et al. (2017), Y. Harikane et al. (2018, 2019), G. Hasinger et al. (2018), M. Scodeggio et al. (2018), B. W. Lyke et al. (2020), Y. Ning et al. (2020, 2022), and Y. Ono et al. (2021) (see details in S. Kikuta et al. 2023). All the number densities presented in this figure, including the spectroscopic values, are corrected for photometric detection completeness.
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 = 2.2. The circles, squares, upward triangles, diamonds, stars, and pentagons with bars represent the number densities and corresponding error bars from this work, P. Cassata et al. (2011), Y. Zhang et al. (2021), A. Konno et al. (2016), D. Sobral et al. (2017), and K. Ma et al. (2024), respectively. Filled (open) symbols are used (not used) to fit the Lyα LFs. The median of the fitted DPL + DPL and Schechter + DPL functions at each luminosity is shown as red solid and black dashed lines, respectively. The 68th percentile range for the fitted DPL + DPL and Schechter + DPL functions at each luminosity is shown as red and gray shading, respectively. The red dotted–dashed line represents the median of the galaxy component for the DPL + DPL function.
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 = 4.9. The circles, squares, and upward triangles with bars represent the number densities and corresponding error bars from this work, A. B. Drake et al. (2017), and G. de La Vieuville et al. (2019), respectively. Filled (open) symbols are used (not used) to fit the Lyα LFs. The median of the fitted DPL and Schechter functions at each luminosity is shown as red solid and black dashed lines, respectively. The 68th percentile range for the fitted DPL and Schechter functions at each luminosity is shown as red and gray shading, 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: Photometrically derived rest-frame equivalent width distribution of our LAE sample at z ∼ 2.2, 3.3, 4.9, 5.7, and 6.6. Gray histograms represent the normalized probability density p(EW0) of our LAE sample. The red solid lines in each panel represent the best-fit exponential distribution fitted in the range of EW0 = 40−200 Å.
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: Transmission curves of Subaru/HSC broadband and narrowband filters. The black lines represent the curves for the broadband filters (g, r2, i2, z, and y). Note that the r- and i-band filters were replaced with the new r2 and i2 filters in 2016. For simplicity, we refer to them as the r and i bands. The purple, blue, pale blue, yellow, orange, pink, and red lines represent the curves for the NB387, NB527, NB718, NB816, NB921, NB973, and NB1010 narrowband filters, respectively. The value written after the band names corresponds to the redshift of LAE samples.
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 = 3.3. The circles, squares, upward triangles, diamonds, and stars with bars represent the number densities and corresponding error bars from this work, A. B. Drake et al. (2017), M. Ouchi et al. (2008), G. de La Vieuville et al. (2019), and T. T. Thai et al. (2023), respectively. Filled (open) symbols are used (not used) to fit the Lyα LFs. Downward arrows in Figures 6–11 represent the 1σ upper-limit values. The lines and shading represent the same statistics described in Figure 5.
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: (Top) Detection completeness ﹩{f}_{{\rm{\det }}}﹩ of our narrowband images taken with Subaru/HSC in the UD-COSMOS field. The x-axis (i.e., NB [mag]) represents the total narrowband magnitude. The purple, blue, pale blue, yellow, orange, pink, and red lines represent ﹩{f}_{{\rm{\det }}}﹩ at each narrowband magnitude for the NB387, NB527, NB718, NB816, NB921, NB973, and NB1010 images, respectively. (Bottom) ﹩{f}_{{\rm{\det }}}﹩ of our NB816. The blue, orange, red, yellow, pale blue, and purple lines represent ﹩{f}_{{\rm{\det }}}﹩ in the UD-COSMOS, D-COSMOS, UD-SXDS, D-SXDS, D-DEEP23, and D-ELAISN1 fields, 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 = 5.7. The circles, squares, upward triangles, diamonds, stars, pentagons, downward triangles, crosses, and hexagons with bars represent the number densities and corresponding error bars from this work, A. B. Drake et al. (2017), M. Ouchi et al. (2008), A. Konno et al. (2018), S. Santos et al. (2016), A. J. Taylor et al. (2021), E. C. Herenz et al. (2019), G. de La Vieuville et al. (2019), and T. T. Thai et al. (2023), 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: An example of type 1 AGN excluded by an F-test. In the top of each panel, the solid dark green line shows the line spectrum after subtracting starlight determined from the host galaxy with Plate-Mjd-Fiberid shown in the top-left corner. The solid red line represents the best-fitting results with ﹩{\chi }_{1}^{2}/{{\rm{dof}}}_{1}﹩ (﹩{\chi }_{2}^{2}/{{\rm{dof}}}_{2}﹩) of two (one) narrow Gaussian functions for each core component of the [O III] doublet. The dashed cyan line represents continuum emission, the solid green lines represent broad Hβ emission line, and the solid cyan lines represent extended [O III] components. The dashed blue and red lines (in the top-left panel) represent the blueshifted and redshifted components of [O III], respectively. The dashed blue line (in the top-right panel) represents the single peak of [O III]. 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.