adsabs/AstroCLIMB huggingface dataset:
Paper: Buildup, Explosion, and Untwisting of a Solar Active Region Jet Observed with Solar Orbiter, IRIS, and SDO
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore, Sanjiv K. Tiwari, David Berghmans, Andrei Zhukov, Marilena Mierla, Cis Verbeeck, Koen Stegen
Figure caption: Active region (AR) jet observed on 2023 March 29 (NOAA 13262). Panel (a) shows an HRIEUV 174 Å image of the AR coronal jet. Panels (b) and (c), respectively, show an SDO/AIA 171 Å image and an IRIS 1400 Å SJI of the same jet. Panel (d) shows an SDO/HMI magnetogram of the AR jet-base region. The white box shows the field of view (FOV) in Figures 3, 4, and 5. HMI contours, of levels ±50, 100 G, at 14:15:29 UT are overlaid in panel (b), where red and cyan contours outline positive and negative magnetic fluxes, respectively.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: The same as Figure 1 but for high- (A), (B), (C), (D) and low-latitude (E), (F), (G), (H) measurements by Ulysses.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Latitudinal (Δθ) and longitudinal (Δϕ) deviations of photospheric footpoints among the different source surfaces of the PFSS model for Ulysses midlatitude (up panels) and Wind ecliptic (down panels) measurements.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: The same as Figure 3 but for high- and low-latitude measurements by Ulysses.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Photospheric footpoints traced from the different source surfaces of the PFSS model on the GONG synoptic magnetogram and EUVI synoptic map.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Latitudinal (Δθ) and longitudinal (Δϕ) deviations of photospheric footpoints among the PFSS, PFCS, and CSSS models for Ulysses high-(up panels) and low-latitude (down panels) measurements.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: The same as Figure 2 but for high- and low-latitude measurements by Ulysses.
Paper: Backmapping of the High- and Low-latitude Solar Wind under Multiple Heliospheric and Coronal Magnetic Field Configurations
Authors: Xinyi Ma, Liping Yang, Xueshang Feng, Hui Tian, Honghong Wu, Fang Shen, Wangning Zhang, Mengxuan Ma, Xiao Zhang, Ziwei Wang
Figure caption: Observed and predicted HMF polarity and strength with in situ measurements obtained from Ulysses and Wind.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Emissivity in the Z-midplane that would be detected in the 193 Å channel of AIA at t = 440 minutes, showing clusters with a distribution of sizes as outlined by the green boxes. The dashed green box marks the largest cluster and area of the spatially averaged light curve in Figure 11.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: 193 Å intensity profiles (emission integrated along the LOS as a function of position) corresponding to an observation made from the top (red) and from the right (blue) of Figure 9. The dashed vertical lines indicate approximate FWHMs in the red intensity profile that correspond to the clusters identified in the green boxes in Figure 9.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Left: iso-surfaces of Jz current density at ±2 × 10−3 Am−2, showing the many thin elongated current sheets that have formed at t = 300 minutes. Blue/red corresponds to negative/positive Jz. Right: iso-surfaces of temperature at t = 300 minutes, showing coronal plasma at 2 MK.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Magnitude of the horizontal velocity on the bottom photospheric boundary at three different times during a driving period. The top and bottom panels show times when each of the two 6 × 6 arrays reach their maximum value, while the other is at minimum. The middle panel shows an intermediate time when the two arrays temporally overlap.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: SDO/AIA temperature response functions for the four channels used throughout this paper: 171 Å (red), 193 Å (orange), 94 Å (green), and 335 Å (blue).
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Radial profile of a single rotational cell at a time of maximum velocity normalized by vpeak = 7.5 km s−1.
Paper: Self-Consistent Heating of the Magnetically Closed Solar Corona: Generation of Nanoflares, Thermodynamic Response of the Plasma and Observational Signatures
Authors: Craig D. Johnston, Lars K. S. Daldorff, James A. Klimchuk, Shanwlee Sow Mondal, Will T. Barnes, James E. Leake, Jack Reid, Jacob D. Parker
Figure caption: Trajectories of 9 randomly selected footpoints in the bottom photospheric boundary over 15 periods of driving from t = 0–300 minutes.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Scatter plots showing the logarithm of the masses in the CORSET, GCS, DP1, DP2, and DP3 data sets. We include separate panels for the STA and STB results where appropriate. The color of each panel indicates whether the pairing combines the same or different methods and satellite viewpoints as shown in the legend.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Graphic representations of the expected coverage in longitude given different locations of a pair of satellites. The top left panel shows the longitudes well-observed by A (red), B (blue), or both (purple) versus the longitude of A and B. The dashed lines show the location of Earth (black) and the two satellites (red and blue). The top right shows the same information but with the y-axis rearranged to show percent coverage instead of the specific longitudes covered. The bottom two rows show the longitudes covered from a top down perspective. The satellite locations are at 40°, 60°, and 80° from left to right in these rows. The top row of circle plots includes only the views from A and B but the bottom row accounts for a satellite at L1/Earth by including gray shading.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Second example of a catalog event in the same format as Figure 2. The top two rows show COR2 mass images (STB left, STA right), with overlays of the CORSET (red) mask. The bottom left panel shows the Solar Mach overview of the geometry with the reference longitude indicating the CME longitude. The bottom left shows the evolution of the CORSET masses.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Scatter plots comparing the longitude (top left) and latitude (bottom right) for different pairs of data sets, analogous to Figure 7. The light gray lines show differences of ±30° in longitude and ±10° in latitude.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Separation between a CME and the PoS versus separation between the two STEREO satellites. Each point is colored according to the mass ratio between the two perspectives (smaller divided by larger mass).
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Histograms of the probability density of the logarithmic mass within each data set. The label lists the set name and the number of data points.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Third example of a catalog event in the same format as Figure 11. This event includes GCS reconstructions, unlike Figure 11.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Longitudinal coverage for a cutoff value of 40°.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Longitudinal coverage for a cutoff value of 60°.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Schematic illustration of possible scenarios that may explain the shallower-than-expected slope of the torus size–luminosity relation. The top row shows the effects of anisotropic disk emission and torus geometry in low-luminosity (left) and high-luminosity (right) AGNs. The middle row shows a large inner radius (left) and a small inner radius (right) in the tori of recently dimmed and brightened AGNs, respectively. The bottom row shows the geometry of a slim accretion disk, where the torus clouds receive less radiation due to self-shadowing. The figure is not to scale.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: The Hβ BLR size from S. Wang & J.-H. Woo (2024) plotted against the torus (Rtor) in the W1 band (left) and W2 band (right). The green solid line shows our best-fit regression, and the shaded region corresponds to the 1σ –3σ confidence intervals around the best-fit line. The orange dotted–dashed lines indicate results from optical/NIR interferometry presented by Gravity Collaboration et al. (2023).
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: The top row shows the relationship between Rtor,W1 and L5100 for three Eddington ratio bins in the W1 band (left) and the corresponding deviation values (defined as ﹩{\rm{\Delta }}\mathrm{log}\,{R}_{\mathrm{tor}}=\mathrm{log}\,({R}_{\mathrm{tor},\mathrm{obs}}/{R}_{\mathrm{tor},\mathrm{pred}})﹩) as a function of the Eddington ratio (right). The shaded region indicates the highest bin of Eddington ratio. The bottom row presents the same relationships for the W2 band. A negative trend is evident in the right panels, where deviation values decrease as the Eddington ratio increases for both bands.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Size of torus (Rtor) from RM in the W1 band (left) and the W2 band (right) versus MIR W2 luminosity. The green solid line represents our best-fit regression with a free slope. The shaded region corresponds to the 1σ–3σ confidence intervals around the best-fit relation. The black dashed lines show the best fit with a fixed slope of 0.5. The purple dotted–dashed lines indicate regression results from A. K. Mandal et al. (2024).
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: The map of the critical magnetic relaxation (δmag,cri) required to produce high-J attractors for the different RAT models (﹩{q}^{{\rm{\max }}}﹩) and the angle between radiation direction with the magnetic field (ψ) in the different radiation fields of U = 1–104 (panels (a)–(d)). The gray shaded areas denote the parameter space where high-J attractors can be produced by RATs only, no need for magnetic relaxation. The contour levels show some values of δmag,cri. The critical magnetic relaxation strength must be increased to have universal high-J attractors in stronger radiation fields.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: The phase trajectory map for the RAT model of ﹩{q}^{{\rm{\max }}}=3﹩ and PM grains of δmag = 1 in the RD regime of different U/(n1T2) (panels (a)–(c)). Some grains are rapidly spun up to the high-J attractor, but the majority of grains are driven to low-J attractors and trapped at low-J rotation. Collisional and magnetic excitations are insufficient to significantly scatter grain orientations to transport them to high-J attractors compared to the CD regime, and grains are trapped by RATs.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Phase trajectory maps for PM grains of δmag = 1 and the RAT model of ﹩{q}^{{\rm{\max }}}=3﹩ in CD regime of different U/(n1T2) (panels (a)–(c)). Grains are eventually aligned at high-J attractors by RATs due to collisional and magnetic excitations.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Phase trajectory maps for the RAT model of ﹩{q}^{{\rm{\max }}}=3﹩ and SPM grains of δmag = 103 in extreme radiation fields (panels (a)–(d)). The fraction of grains that have fast alignment at high-J attractor decreases with increasing U/(n1T2) due to reduced efficiency of magnetic relaxation.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 25 but for the time-dependent alignment. Grain alignment degrees slowly increase with time and reach perfect alignment after 50–100τdamp.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 31 but for the time-dependent grain alignment degrees. The net grain alignment degree (R) decreases with increasing U/(n1T2) due to reduced efficiency of magnetic relaxation.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 23 but for temporal evolution of the alignment degrees for δmag = 103. Alignment degrees increase rapidly within 0.01τdamp and become saturated at R ∼ 0.45 for intense radiation due to RAT trapping.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 27 but for ﹩{q}^{{\rm{\max }}}=1﹩. Grains have no high-J attractors and undergo a random trajectory at thermal rotation and deterministic trajectories at suprathermal rotation of J/I1ωT > 3.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 27 but for time-dependent alignment. Alignment degree increases rapidly within 0.01τdamp and becomes saturated at R ∼ 0.2 for intense radiation due to RAT trapping.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 29 but for time-dependent alignment. Grains have negligible alignment due to the lack of a high-J attractor.
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: CMD of our DESI Draco sample. The region inside the dashed lines is the color selection for the Draco candidates sample from the DESI DR1 Stellar Catalog data. For the color–magnitude cuts used in the selection, we use an old, metal-poor ([Fe/H] = −1.5 dex) Dartmouth isochrone with an age = 10 Gyr (A. Dotter et al. 2008) and select stars within ±0.39 mag of the isochrone g − r value. We use Legacy survey (A. Dey et al. 2019) photometry of the M92 globular cluster to define a region for the horizontal branch, since that is not included in the isochrone. The data sample after the color cut is labeled in red triangles, and the final selected data sample (see Section 2.1) is labeled in blue circles.
Paper: Beyond MESA Defaults: The Impact of Structural Resolution Uncertainty in p-mode Asteroseismology
Authors: Yaguang Li, 亚光 李, Meridith Joyce
Figure caption: Differences in stellar parameters (age, R, and fΔν, from top row to bottom row, respectively) when evaluated against the same oscillation frequency for the two tracks with different delta_mesh_coeff. The left columns show tracks with varying mass, and the right columns show those with varying metallicity.
Paper: Beyond MESA Defaults: The Impact of Structural Resolution Uncertainty in p-mode Asteroseismology
Authors: Yaguang Li, 亚光 李, Meridith Joyce
Figure caption: Results of resolution tests, showing differences in frequency or period, εdmesh or ζdmesh (see Equations (3) and (5)), calculated using alternative delta_mesh_coeff values to compare with the default delta_mesh_coeff = 1.0.
Paper: Beyond MESA Defaults: The Impact of Structural Resolution Uncertainty in p-mode Asteroseismology
Authors: Yaguang Li, 亚光 李, Meridith Joyce
Figure caption: Seismic ratios (r01 and r13) vs. Δν for low-mass MS models. The bottom panels show the residuals between the two delta_mesh_coeff tracks.
Paper: Beyond MESA Defaults: The Impact of Structural Resolution Uncertainty in p-mode Asteroseismology
Authors: Yaguang Li, 亚光 李, Meridith Joyce
Figure caption: P-mode phase offset ϵp vs. Δν for low-mass MS models. The bottom panels show the residuals between the two delta_mesh_coeff tracks.
Paper: Beyond MESA Defaults: The Impact of Structural Resolution Uncertainty in p-mode Asteroseismology
Authors: Yaguang Li, 亚光 李, Meridith Joyce
Figure caption: Seismic H-R diagram (νmax vs. Teff) around the RGBB (top panel) and the CHeB phase (bottom panel).
Paper: Beyond MESA Defaults: The Impact of Structural Resolution Uncertainty in p-mode Asteroseismology
Authors: Yaguang Li, 亚光 李, Meridith Joyce
Figure caption: Seismic ΔΠ1–Δν diagram for the RGB (top panel) and CHeB (bottom panel) phases.
Paper: Beyond MESA Defaults: The Impact of Structural Resolution Uncertainty in p-mode Asteroseismology
Authors: Yaguang Li, 亚光 李, Meridith Joyce
Figure caption: Evolutionary tracks used in this studied color coded by the primary EEP values. The black dots show the critical points that separate primary EEPs.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Top: lag analysis result for Mrk 335, shown as an example of a detrended target. The top panel shows intercalibrated optical light curves, with the gray-shaded regions representing the DRW model from PyCALI. The middle panel presents accretion-disk-corrected MIR light curves in the WISE W1 and W2 bands. The blue and red points represent the scaled optical light curves shifted by the τcent from ICCF relative to the W1 and W2 light curves, respectively. The dashed lines show the first-order polynomial fit on light curves. The bottom-left panel shows the ICCF (black curve) and CCCD (blue histogram) for W1. The hatched region below the ICCF curve indicates where r ≥ 0.8 ﹩{r}_{\max }﹩. The best-fit transfer function derived from the MICA analysis is shown in blue, with the shaded region indicating uncertainties. The bottom-right panel shows W2 data, mirroring the left panel.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Size of torus (Rtor) as a function of 5100 Å luminosity for W1 (left) and W2 (right). The green solid line represents our best-fit regression with a free slope. Shaded regions represent the 1σ, 2σ, and 3σ confidence intervals around the best-fit regression line, derived from the percentiles of model predictions sampled from the posterior distributions of slope and intercept (hereafter, this method is applied in all related figures). The black dashed lines represent the best-fit model with a fixed slope of 0.5, while the purple lines show the regression results from A. K. Mandal et al. (2024).
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: The distribution of 5100 Å continuum luminosity for variable AGNs with (blue) and without (red) measured lags. The black dashed line indicates the luminosity at which a lag of ∼180 days is expected, corresponding to the WISE cadence.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Distribution of ﹩p({r}_{{\rm{\max }}})﹩ versus ﹩{r}_{{\rm{\max }}}﹩ for W1 (left) and W2 (right). Blue circles represent the Hβ RM literature sample, and red circles represent SAMP AGNs. The black dashed lines indicate the selection criteria of ﹩p({r}_{{\rm{\max }}})=0.1﹩ versus ﹩{r}_{{\rm{\max }}}=0.6﹩. Targets that do not meet these criteria are presented as open circles.