adsabs/AstroCLIMB huggingface dataset:
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The left panel shows Type 1 and Type 2 AGNs in the BPT diagram for O3HB vs. N2HA. The contour filled with bluish colors represents the results for all the narrow emission-line galaxies collected from SDSS DR12. The contour with levels as solid reddish lines and dotted reddish lines represent the results for the Type 2 and Type 1 AGNs with reliable stellar velocity dispersions in this work, respectively. Thick pluses in red and green mark the central positions of the contours for the Type 2 and Type 1 AGNs, respectively. The solid purple line and solid dark green line show the dividing lines between different kinds of narrow emission-line galaxies in Kewley et al. (2006) and Kauffmann et al. (2003a). Dashed cyan lines mark the strip applied to collect the Type 2 and Type 1 AGNs to check in a simple manner the effects of AGN activities on stellar velocity dispersion comparisons. The right panel shows results similar to Figure 11, but for the 1044 Type 1 AGNs and the 4202 Type 2 AGNs covered by the strip shown in the left panel. The symbols and line styles have the same meanings as those in Figure 11.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Similar to Figure 11, but for the 1445 Type 1 AGNs and the 1445 Type 2 AGNs in the subsamples that have the same distributions of z, O3HB, N2HA, and L O3. The symbols and line styles have the same meanings as those in Figure 11.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The left panel shows the dependence of σ on L O3/σ 4 for Type 1 AGNs (contour filled with bluish colors) and Type 2 AGNs (contour levels by reddish lines). The solid red line and dashed red lines are for the best-fitting results and the corresponding 5σ confidence bands for Type 1 AGNs. The solid blue line and dashed blue lines are for the best-fitting results and the corresponding 5σ confidence bands for Type 2 AGNs. The right panel shows the L O3/σ 4 distributions of Type 1 AGNs (histogram filled with blue lines) and Type 2 AGNs (histogram filled with red lines).
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Bolometric luminosity distributions of the 1445 Type 1 AGNs (histogram filled with blue lines) and the 1445 Type 2 AGNs (histogram filled with red lines) in the subsamples, which have the same distributions of z, O3HB, N2HA, and L O3. Dashed lines in purple and in cyan represent the corresponding best-fitting Gaussian profiles for the distributions of the Type 2 and Type 1 AGNs, respectively.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The mean spectra around 8500 Å of the Type 1 AGNs without (left panel) and with (right panel) apparent absorption features around 4000 Å. The solid red line shows the best-fitting results for the Ca II triplet. The measured stellar velocity dispersion from the Ca II triplet is marked in red in each panel.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: These are two examples of K2 flare search results. The left panels are an example of 1-minute data, and the right panels are an example of 30-minute data.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: These two pictures show the distribution of the EW of Hα of flare and nonflare stars for low-resolution (left panel) and medium-resolution spectra (right panel). Red circles represent flare stars, and black circles represent nonflare stars.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Flare-frequency distributions of TESS, Kepler 1 minute, Kepler 30 minutes, and K2, where different colors represents different stellar temperature regions.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Relationship between our obtained orbital parameters and published data, where the left panel is the sum of the radius, the middle panel is the period, and the right panel is the ratio of the radius of exoplanet and host stars. The red lines represent the linear fit.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: The observational and theoretical light curves, where the circles represent the observation data, and the red line is the fitted result. Left panels are the fitting of the whole light curve. Right panels are one eclipse fitting.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Examples of transit light curves with flares, where the left panel is the fitting of the whole light curve and the right panel is one eclipse fitting.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The left panel shows the distributions of the stellar velocity dispersions of the 6260 Type 1 AGNs (histogram filled with blue lines) and the 15,353 Type 2 AGNs (histogram filled with red lines), respectively. The right panel shows the distributions of high-quality stellar velocity dispersions (10 times larger than their uncertainties) of 1680 Type 1 AGNs (histogram filled with blue lines) and 8535 Type 2 AGNs (histogram filled with red lines), respectively. In each panel, dashed lines in purple and in cyan represent the corresponding best-fitting Gaussian profiles for the ﹩\mathrm{log}(\sigma )﹩ distributions of Type 2 and Type 1 AGNs, respectively.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The top-left panel shows the distributions of σ/σ O3 of our measured stellar velocity dispersions σ to the core [O III] line width σ O3 in the 6260 Type 1 AGNs and in the 15,353 Type 2 AGNs in the main samples. The top-right panel shows distributions of σ O3 in the 6260 Type 1 AGNs and in the 15,353 Type 2 AGNs in the main samples. The bottom-left panel shows the distributions of σ/σ O3 in the 5468 Type 1 AGNs and in the 5468 Type 2 AGNs in the subsamples that have the same distributions of σ/σ O3. The bottom-right panel shows the distributions of σ O3 in the 5468 Type 1 AGNs and 5468 Type 2 AGNs in the subsamples that have the same distributions of σ/σ O3. In each panel, the histogram filled by blue lines and red lines show the distributions of Type 1 and Type 2 AGNs, respectively, and the dashed line in purple and in cyan represent the corresponding best-fitting Gaussian profiles for the distributions of Type 2 AGNs and the Type 1 AGNs, respectively. In the bottom-left panel, the significance level provided by the Kolmogorov–Smirnov statistic technique is marked in red.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Correlations between the measured stellar velocity dispersions σ after correcting for instrument resolutions and the reported σ  bt15 (in blue color) of the 39 Type 1 AGNs in Bennert et al. (2015), between σ and σ  bt21 (in red color) of the 37 Type 1 AGNs in Bennert et al. (2021), and the reported σ  xb11 (in green color) of the 2 Type 1 AGNs in Xiao et al. (2011) and the reported σ  hb12 (in dark green color) of the 5 Type 1 AGNs in Harris et al. (2012). The solid blue line and dashed blue lines show the best-fitting results to the correlation between σ  bt15 and the measured σ in the article after correcting instrument resolutions, and the corresponding 99.9% confidence bands. The solid red line and dashed red lines show the best-fitting results to the correlation between σ  bt21 and the measured σ in the article after correcting for instrument resolutions, and the corresponding 99.9% confidence bands.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The left panel shows the dependence of σ on the total [O III] line luminosity L O3 of the 6260 Type 1 AGNs with a well-measured σ. The solid red line and dashed red lines show the best-fitting results and the corresponding 5σ confidence bands, respectively. The right panel shows the L O3 distributions of the Type 1 AGNs with (histogram filled with red lines) and without (histogram filled with blue lines) apparent absorption features around 4000 Å. Dashed lines in purple and in cyan represent the corresponding best-fitting Gaussian profiles for the L O3 distributions of Type 1 AGNs with and without measured stellar velocity dispersions, respectively.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Correlation between σ and σ CaII for the 72 Type 1 AGNs with high-quality Ca II triplets. The solid red line and dashed red lines show the best-fitting results and the corresponding 99.99% confidence bands, and the solid blue line shows σ = σ CaII.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Best-fitting results (solid red line) to Ca II triplets (solid dark green line) of the 72 Type 1 AGNs. The stellar velocity dispersion σ CaII measured from Ca II triplets and the σ from absorption features around 4000 Å are marked in red in each panel.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The inverse-variance-weighted mean spectra of Type 1 AGNs (solid dark green line) with stellar velocity dispersions well measured from absorption features around 4000 Å and of the other Type 1 AGNs (solid red line) without apparent absorption features around 4000 Å.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: Examples of the spectral fitting for a low-redshift quasar observed by LJT (a) and a high-redshift quasar observed by P200 (b). Black lines denote the total dereddened spectra, yellow lines denote the continua (f pl + f poly), cyan lines denote the Fe II templates (f Fe II ), blue lines denote the whole emission lines, red lines denote the broad-line components, and green lines denote the narrow-line components. For a spectrum that is successfully decomposed into a host-galaxy component and a pure quasar component, the purple line denotes the host component, the gray line denotes the pure quasar component, and the pink line denotes the spectrum reconstructed from the PCA host and quasar components.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: The absolute magnitudes M  i (z = 2) and redshift distributions of our identified GPQs and the whole GPQ candidate catalog. In the main panel (lower left), our identified GPQs are represented by orange triangles, and the two-dimensional histogram (density plot) of the GPQ candidate catalog is shown in the background. White contour lines based on two-dimensional kernel density estimation (KDE) are displayed on the density plot. In the top and right panels, the blue shaded areas denote the KDE probability density functions of the GPQ candidate catalog, and the orange bars denote the probability densities of our identified GPQs.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: Log-scale histograms of the apparent i  P1 magnitudes of our identified GPQs (orange bars) and the whole GPQ candidate catalog (filled blue step plot).
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: The sky distribution of the 204 spectroscopically identified GPQs (red squares) in Galactic coordinates. A HEALPix (Górski et al. 2005) sky density map of known Type 1 QSOs and AGNs from MILLIQUAS v7.4d is shown in the background, with the parameter N side = 64 and an area of 0.839 deg2 per pixel.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: Flowchart of the spectral-fitting process with PyQSOFit and QSOFITMORE.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Photometric metallicities predicted by our model ensemble ([Fe/H] G ) for the G-band target data set, plotted against the corresponding metallicity estimates from the Gaia DR2 RR Lyrae catalog ([Fe/H]DR2; left), and by the IB21 formula ([Fe/H]IB21; middle). The pulsation periods are color coded; the red line denotes the identity function. Right: histograms and corresponding kernel density estimates of the same data set as in the left and middle panels. Green: [Fe/H] G  estimates from this work, blue: IB21 metallicities, red: [Fe/H] values from the DR2 RR Lyrae catalog.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Left: photometric metallicities predicted by our model ensemble ([Fe/H]﹩{}_{{K}_{s}}﹩) for the K  s -band target data set, plotted against metallicity estimates by the H18 method ([Fe/H]H18). The pulsation periods are color coded; the red line denotes the identity function. Right: histograms and corresponding kernel density estimates of [Fe/H]﹩{}_{{K}_{s}}﹩ (green) and [Fe/H]H18 (blue) values for the target data set, and [Fe/H] I  values for the development data set (gray).
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Predicted vs. true photometric metallicities from the best-performing predictive models for the K  s  (left) and G (right) wave bands. The top and bottom panels show the full training and validation data sets, respectively. The red lines denote the identity function.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Distributions of the metallicities of the K  s -band (left) and G-band (right) development data sets and their sample weights. Red bars and blue curves show the histograms and kernel density estimates of the [Fe/H] I  values, respectively. Black symbols denote the (normalized) weights computed from the inverse of the density. Red points show the final sample weights.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Celestial distribution of the target data set of our Gaia K  s -band photometric metallicity estimator in the Galactic coordinate system. The predicted [Fe/H]﹩{}_{{K}_{s}}﹩ values are color coded.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption:  G-band mean [Fe/H] predictions of 60 RRab stars by our LSTM model ensemble plotted against the individual HDS metallicity measurements of the same objects. The red line denotes the identity function.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Celestial distribution of the target data set of our Gaia G-band photometric metallicity estimator in the Galactic coordinate system. The predicted [Fe/H] G  values are color coded.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Schematic architectural graph of our predictive models. Gray filled boxes represent neural network (LSTM and dense) units; open boxes denote their inputs and outputs. The activation vector at the output of the first biLSTM layer is 64 and 32-dimensional for the K  s - and G-band model, respectively.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Histograms of the true (red) and predicted (gray) [Fe/H] values from our K  s - and G-band model ensembles for the training (T; left) and validation (V; right) data sets. The top and bottom panels show the histograms on logarithmic and linear scales, respectively.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Left panels show the best descriptions (solid red line) determined using the SSP method for the SDSS spectra (solid dark green line) of the Type 1 AGN 0997-52734-0303 and Type 2 AGN 0332-52367-0317 shown in Figure 1. In each left panel, from left to right, the vertical purple lines point out the emission lines being masked out when the SSP method is running, including [O II] λ3727, Hθ, Hη, [Ne III] λ3869, He I λ3891, Ca K, [Ne III] λ3968, Ca H line, [S II] λ4070, Hδ, Hγ, [O III] λ4364, He I λ5877, and the [O I] λλ6300, 6363 doublet, and the area filled by purple lines around 5000 Å shows the region masked out including the optical Fe II lines, broad and narrow Hβ and [O III] doublet, and the area filled by purple lines around 6550 Å shows the region masked out including the broad and narrow Hα, [N II],  and [S II] λ6716 doublets. In the top-left panel, the solid blue line shows the determined host-galaxy contributions, and the solid cyan line shows the determined AGN continuum emissions in the Type 1 AGNs. Right panels show the best descriptions (solid red line) of the emission lines around Hα (solid dark green line) after subtracting the host-galaxy contributions. In each right panel, the solid blue line shows the determined narrow Hα, solid purple lines show the determined [N II] doublet, solid pink lines show the determined [O I] doublet, and solid cyan lines show the determined [S II] doublet. In the top-right panel, the solid green lines show the determined broad Gaussian components in the broad Hα, and the dashed blue line shows the determined power-law continuum emissions underneath the emission lines.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Two examples of the best-fitting results (solid red line) to the absorption features around 4000 Å (solid dark green line) in the Type 1 AGN 0997-52734-0303 (PLATE-MJD-FIBERID) (top panels) and in the Type 2 AGN 0332-52367-0317 (bottom panels). In each left panel, the measured stellar velocity dispersion σ and corresponding calculated χ 2 value (summed squared residuals divided by the degrees of freedom) are marked in the top-left corner. In the right panels, the solid dark green lines show the entire observed optical spectrum of the Type 1 AGN 0997-52734-0303 and the Type 2 AGN 0332-52367-0317. The apparent broad Hα  in the Type 1 AGN 0997-52734-0303 is marked in the top-right panel.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The left panel shows an example of an artificial spectrum around 4000 Å (solid line in dark green) considering contributions of AGN continuum emissions (solid blue line) and broad-line emissions (solid purple lines), and the corresponding best-fitting results (solid red line). In the left panel, the solid cyan line shows the spectrum S 2(λ) around 4000 Å collected from the Type 2 AGN SDSS 0789-52342-0246. The right panel shows the correlation between the intrinsic σ  i  and the artificial σ  a . In the right panel, the symbols in blue are for all the data points with artificial σ  a  five times larger than their corresponding uncertainties, and the symbols in red are for the high-quality data points with artificial σ  a  10 times larger than their corresponding uncertainties and χ 2 smaller than 2, the solid red line shows X = Y, and the solid green lines show the 99.99% confidence bands to the linear correlation X = Y.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Best-fitting results (solid red line) to the absorption features around 4000 Å (solid dark green line) of the 41 Type 1 AGNs included in the sample of Bennert et al. (2015) and in the sample of Bennert et al. (2021), and the 2 Type 1 AGNs from the sample of Xiao et al. (2011) and 5 Type 1 AGNs from the sample of Harris et al. (2012). The measured stellar velocity dispersion σ in this article after correcting for instrument resolutions and the reported value σ  bt15 in Bennert et al. (2015) and/or σ  bt21 in Bennert et al. (2021), or σ  xb11 in Xiao et al. (2011), or σ  hb12 in Harris et al. (2012) are marked in red in each panel.