adsabs/AstroCLIMB huggingface dataset:
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: (Left) Final profiles of mass fractions and nuclear energy generation rate at t = 12 μs, and (right) parallel validation results using the negative inverse log form of X  k  as input for both DNNs. Note that each point in the profile plot is every five data points on the grid in the y-direction.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Solutions to the sine wave problem at final time t = 12 μs using a machine-learning model trained using data from the V-shape problem. (a) Contour plots of species mass fractions and nuclear energy generation rate. Each pair of contour plots shows the Strang solution using VODE on the left and the trained DNN model on the right along the vertical dashed line. (b) Profiles along the vertical line.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: A CMD showing Cepheid candidate selection. Magenta lines indicate the initial selection boundary, chosen to encompass the expected Cepheid instability strip while avoiding possible contamination from the dense red giant branch stars. Blue and red points show our final Cepheid sample and rejected outliers, respectively. Representative error bars are shown. The expected mean Cepheid instability strip location and width for P > 5 days, derived from LMC observations (Riess et al. 2019), are shown with thick and thin black lines, respectively. The green arrow indicates the effect of A  V  = 1 mag. Black dots show only a subset of field stars for visualization purposes.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: Composite light curves of the NGC 4258 Cepheids in eight period bins using F350LP or F555W data (top four rows) and the newly observed (F3–F6) Cepheids of the entire period range in the F555W (bottom left) and F814W (bottom right) bands. Black and blue points indicate archival and new measurements, respectively. Points with uncertainties greater than 0.1 mag were excluded. Red curves show cubic-spline fits. We plot two phase cycles for visualization purposes. A common phase from the Yoachim et al. (2009) templates was imposed.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: Archival (F1 and F2) and new (F3–F6) HST observations of NGC 4258 using ACS (F1–F4) and WFC3 (F5 and F6) overlaid on an i-band Sloan Digital Sky Survey image that is 16.′5 on a side. North is up, and east is to the left.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: The NGC 4258 Cepheid PLRs in F555W, F814W, and W  VI  HST. The solid blue lines indicate the best-fit PLRs, while the dashed blue lines indicate their 1σ scatter.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: Example Cepheid light curves in the new NGC 4258 fields (F3–F6). The blue curves show the best-fit Yoachim et al. (2009) templates. We plot two phase cycles for visualization purposes.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: Comparison of the absolute W  VI  HST PLR zero-points between our (circle) and Riess et al.’s (2019; triangle) results. The solid and dashed blue lines indicate the W  VI  HST-band PLR metallicity dependence determined by Riess et al. (2016) and Breuval et al. (2021), respectively. We note that the Breuval et al. (2021) result is based on ground-based V and I filters, whose response functions are similar but not identical to those of the HST F555W and F814W filters, respectively.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: Top: NGC 4258 distance moduli based on individual Cepheids against the Cepheid oxygen abundances estimated from their radial locations. The red line indicates the best-fit regression result using the entire sample of this work, while the blue line shows the Riess et al. (2016) determination. Bottom: best-fit γ values from samples with various minimum period cuts (black curve), with the gray shaded region indicating their random errors. The solid and dashed blue lines indicate the Riess et al. (2016) and Breuval et al. (2021) determinations, respectively.
Paper: Absolute Calibration of Cepheid Period–Luminosity Relations in NGC 4258
Authors: Wenlong Yuan, Lucas M. Macri, Adam G. Riess, Thomas G. Brink, Stefano Casertano, Alexei V. Filippenko, Samantha L. Hoffmann, Caroline D. Huang, Dan Scolnic
Figure caption: The H II metallicity measurements against their deprojected radial distances from the galactic center. The solid line shows the best-fit linear relation, while the dashed lines indicate the ±1σ scatter.
Paper: Comparison of Two Methods for Deriving the Magnetic Field in a Filament Channel
Authors: T. A. Kucera, M. Luna, T. Török, K. Muglach, J. T. Karpen, C. Downs, X. Sun, B. J. Thompson, H. R. Gilbert
Figure caption: (a) Hα and (b) 171 Å images showing the location of the track used to trace the F2 oscillation. Panels (c)–(e) show intensity as a function of time vs. distance along the track from 05:00 to 15:00 UT on May 30 in Hα (c) and 171 Å ((d) and (e)). In panels (c) and (e), the points used to fit the oscillations are shown with + symbols, and the fits corresponding to the Track A fits listed in Table 2 are shown by the colored lines. Panel (d) is the same as panel (e) but without the annotations to show the 171 Å data more clearly.
Paper: Comparison of Two Methods for Deriving the Magnetic Field in a Filament Channel
Authors: T. A. Kucera, M. Luna, T. Török, K. Muglach, J. T. Karpen, C. Downs, X. Sun, B. J. Thompson, H. R. Gilbert
Figure caption: Tracks used to analyze filament oscillations listed in Table 1 superimposed on a GONG Hα image from May 30. In panel (a), the tracks are color coded to show the start time of the oscillation. In panel (b), the colors correspond to the oscillation period. The length of the track represents the maximum displacement over which the oscillation occurred. The dashed lines show more than one measurement along the same path. The tracks are rotated to align the tracks to the location of the region at 2014 May 30 04:29 UT. Because the filament is above the photosphere, however, tracks from many days apart will not be perfectly aligned.
Paper: Comparison of Two Methods for Deriving the Magnetic Field in a Filament Channel
Authors: T. A. Kucera, M. Luna, T. Török, K. Muglach, J. T. Karpen, C. Downs, X. Sun, B. J. Thompson, H. R. Gilbert
Figure caption: Tracks of oscillations in F2 for May 30 and listed in Table 2, superimposed on a GONG Hα image. The dashed lines show more than one measurement along the same path. (a) Tracks A–D used to measure oscillations. (b) The same tracks, color coded to show the oscillation periods. All tracks are rotated to align with the location of the region at 2014 May 30, 04:29 UT.
Paper: The Dust Sublimation Region of the Type 1 AGN NGC 4151 at a Hundred Microarcsecond Scale as Resolved by the CHARA Array Interferometer
Authors: Makoto Kishimoto, Matthew Anderson, Theo ten Brummelaar, Christopher Farrington, Robert Antonucci, Sebastian Hönig, Florentin Millour, Konrad R. W. Tristram, Gerd Weigelt, Laszlo Sturmann, Judit Sturmann, Gail Schaefer, Nic Scott
Figure caption: Details of the fringe track #04 for NGC 4151 on 2021 April 30, in the same format as in Figure 7.
Paper: The Dust Sublimation Region of the Type 1 AGN NGC 4151 at a Hundred Microarcsecond Scale as Resolved by the CHARA Array Interferometer
Authors: Makoto Kishimoto, Matthew Anderson, Theo ten Brummelaar, Christopher Farrington, Robert Antonucci, Sebastian Hönig, Florentin Millour, Konrad R. W. Tristram, Gerd Weigelt, Laszlo Sturmann, Judit Sturmann, Gail Schaefer, Nic Scott
Figure caption: Details of the fringe track #02 for NGC 4151 on 2021 April 30, in the same format as in Figure 7.
Paper: The Dust Sublimation Region of the Type 1 AGN NGC 4151 at a Hundred Microarcsecond Scale as Resolved by the CHARA Array Interferometer
Authors: Makoto Kishimoto, Matthew Anderson, Theo ten Brummelaar, Christopher Farrington, Robert Antonucci, Sebastian Hönig, Florentin Millour, Konrad R. W. Tristram, Gerd Weigelt, Laszlo Sturmann, Judit Sturmann, Gail Schaefer, Nic Scott
Figure caption: Details of the fringe track #01 for NGC 4151 on 2021 April 30, in the same format as in Figure 7.
Paper: The Dust Sublimation Region of the Type 1 AGN NGC 4151 at a Hundred Microarcsecond Scale as Resolved by the CHARA Array Interferometer
Authors: Makoto Kishimoto, Matthew Anderson, Theo ten Brummelaar, Christopher Farrington, Robert Antonucci, Sebastian Hönig, Florentin Millour, Konrad R. W. Tristram, Gerd Weigelt, Laszlo Sturmann, Judit Sturmann, Gail Schaefer, Nic Scott
Figure caption: Details of the fringe track #03 for NGC 4151 on 2021 April 30, in the same format as in Figure 7.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Upper panel: relative changes of peak counts for the IA samples with θ 0 = 0° and different dispersions σ  θ  as indicated in the legend. The lowIA results are also shown (gray). Lower panel: dependence of (n IA/n noIA − 1) on σ  θ  with different lines for different peak heights as explained in the legend. The vertical dashed line marks the value of σ  θ  ≈ 70° corresponding to γ scale ≈ 0.21 as explained in Appendix A.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Upper panel: 2D satellite orientation angle θ 2D distribution of different samples as measured from  ϵ    s   without adding lensing signals. Lower panel: median (blue) and mean (red) values of ∣θ 2D∣ with the change of θ 3D. The gray horizontal dashed line indicates ∣θ 2D∣ = 45°, and the red and blue vertical dashed lines mark the corresponding values of θ 3D inferred from the intersections of the gray dashed line with the red and blue solid lines, respectively.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Zoom-in convergence maps for a high peak (left) and the satellite orientations of the corresponding cluster (right), with the red dot indicating the center of the cluster. From top to bottom, θ 3D = 0°, 30°, and 60°.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Peak height comparison for matched peaks with the upper and lower panels for highIA and lowIA, respectively. In each panel, the gray points are the scatter plots of the matched peaks, and the red dashed line indicates the 1:1 relation. The blue line shows the median peak values in the considered IA model at different bins based on ν noIA, and the error bars are the 1σ dispersions.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Relative changes of peak counts with respect to the noIA case for different θ 3D for the sample with the Euclid-like redshift distribution.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Fractions of central galaxies. The blue, red, and yellow lines are for all centrals, centrals with satellites, and centrals with more than 10 satellites, respectively.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Relative changes of peak counts for lowIA (blue) and highIA (red) samples in comparison with the noIA case for the Euclid-like sample.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Redshift distributions of the considered galaxy catalogs. The yellow and red histograms are for the KiDS- and Euclid-like samples. The blue one is from the original galaxy sample. The three shaded regions are for redshift bins of [0.91, 1.14], [1.45, 1.60], and [1.94, 2.09], respectively.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Comparisons of the IA impacts for the Euclid-like (gray) and KiDS-like samples. The results from the KiDS-like highIA and lowIA samples are shown in red and blue, respectively.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: The integrated spectra within a radius of 0.″4 from the galactic center of jellyfish galaxies in this study. The left panels show the original spectra before continuum subtraction, and the middle panels show the continuum subtracted spectra. In the middle panels, several strong emission lines are marked in each spectrum. The right zoomed-in panels show the Hα+[N II] region of each galaxy. We plot the observed spectra (blue solid lines), our best-fit models (pink solid lines), and residuals (green solid lines). In the case of AGN host galaxies, we plot narrow and broad components of the emission lines with orange solid lines and red dashed lines, respectively.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: The zoomed-in HST images of the five jellyfish galaxies with sizes of 12″ × 12″. Green boxes show the FOV of the GMOS/IFU 2-slit mode (5″ × 7″). Magenta arrows represent the directions to the cluster center (BCGs). The orientations are the same as in Figure 1.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: HST color images of the host clusters of the jellyfish galaxies in this study. These images were prepared by combining the two band images of HST/ACS F606W and F814W. Cyan circles denote the location of each jellyfish galaxy. Magenta circles denote the brightest cluster galaxy (BCG), which is set to be the center of each cluster. The orientations and the angular scales are marked.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Color–magnitude diagrams of galaxies detected in the HST images of the host clusters. All colors and magnitudes are de-reddened by the foreground extinction magnitudes. Red star symbols show the data of the five jellyfish galaxies. Gray circles show the data of all extended sources with half-light radii larger than 0.″2 in the angular scale and ≳1 kpc in the physical scale.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: CE size as a function of continuum luminosity at 5100 Å. Lag measurements and 1σ errors from other low-redshift continuum RM campaigns (see Table 4) are also shown. The best linear MCMC fit is based on the combined sample assuming a typical luminosity uncertainty of 0.05 dex. The τ–L relation predicted by the RPC model from Netzer (2022) is also displayed without any normalization.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: CE size at 2500 Å as a function of the BH mass. Red and blue dots with 1σ errors denote the ZTF sample and local AGN sample, respectively. Dots with different sizes present the corresponding Eddington ratios, and three examples of ﹩\dot{m}\,=﹩ 0.01, 0.1, and 1 are listed. Different lines (with slope of 2/3 assuming L ∝ M BH following Yu et al. (2020b), slightly different from the real situation) indicates the predictions from the SSD model with Eddington ratios ﹩\dot{m}\,=﹩ 0.01, 0.1, and 1. The orange lines are the best linear fits for the combined samples with slopes of 0.72 (left) and 0.83 (right), assuming the typical error of the BH mass is 0.4 dex.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Upper panel: SDSS spectrum overlapped with the ZTF gri filters. Lower panel: ZTF light curves showing a temporally negative τ gr (r-band leads g-band) around MJD = 58600. The red dashed line indicates the g-band peak, obviously lagging to that of the r band. Also see the overall lag measurements in the first panel of Figure 2.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Relationship between monochromatic luminosity at 5100 Å and ﹩{\dot{m}}^{1/3}{M}_{\mathrm{BH}}^{1/3}﹩. The blue dots are the local AGN, and red dots represent the parent sample and core sample in different panels. The black lines are the best linear fits.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Distributions of CE size at 8000 Å for different samples. The self-gravity limit of R sg = 12 days is indicated by the black dashed line. Different samples are labeled with different lines.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: The II correlations measured from our IA samples with θ 0 = 0° and different σ  θ  without adding shear signals. Colored lines with error bars are the results of different σ  θ  as indicated in the legend, where, e.g., 0 for σ  θ  = 0° and 030 for σ  θ  = 30°. The black line is the theoretical NLA prediction with A IA = 0.98.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Upper panels: simulation results of the relative peak count differences for the three narrow redshift bin samples of the highIA case (left) and for the z ∼ 1 sample with different θ 3D (right). Lower panels: corresponding results from the Gaussian model calculations.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Fractions of matched (dotted), newly born (solid), and disappeared (dashed) peaks in κ noIA bins for the Euclid-like sample. The red, green, and blue lines are for highIA, θ 3D = 30°, and lowIA cases, respectively. Shaded regions are excluded from the analyses because of the very low peak numbers there resulting in large fluctuations.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Results from the empirical fitting model (dashed lines) in comparison with those from simulations (solid lines). The upper panel is for the highIA (red), θ 3D = 30° (green), and lowIA (blue) cases, and the lower panel is for θ 0 = 0° and σ  θ  = 10° (red) and 60° (orange), respectively.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Noise field parameters for the three narrow redshift bin samples with red, orange, and blue lines for z ∼ 1, ∼1.5, and ∼2, respectively. From left to right: ﹩{\sigma }_{0}^{\mathrm{total}}﹩, ﹩{\gamma }_{G}^{\mathrm{total}}﹩, and ﹩{\theta }_{\star }^{\mathrm{total}}﹩. The dotted lines in the left panel indicate the σ 0,noIA of the three samples.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Average peak height shifts Δκ (upper panel) and scatters σ Δκ  (lower panel) in κ noIA bins for the three considered cases: highIA (red), 30° (green), and lowIA (blue). Dots are the results measured from the data, and the solid lines are the fitting results using the parameters listed in Table 1 as described in the text.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Results with different smoothing scale θ  G  as shown in the legend for the Euclid-like sample in the highIA (solid) and lowIA (dotted) cases.
Paper: Effects of Galaxy Intrinsic Alignment on Weak Lensing Peak Statistics
Authors: Tianyu Zhang, Xiangkun Liu, Chengliang Wei, Guoliang Li, Yu Luo, Xi Kang, Zuhui Fan
Figure caption: Dependence of γ scale on σ  θ . The horizontal dashed line indicates γ scale = 0.21, and the red point marks its intersection with the blue line.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Ratio between continuum emission size from observation and SSD prediction as a function of basic AGN properties. In each panel, the binned mean values and 1σ uncertainties are plotted for better demonstration of the correlations. Red dots are ZTF parent/core-sample objects, and blue dots are local AGNs from Table 4. The Spearman correlation results for the P+L and C+L samples are listed in each panel. Black dashed and dotted lines indicate d ratio = 1 and 3, respectively.