adsabs/AstroCLIMB huggingface dataset:
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Error in the measured accretion rate (with respect to the analytical Bondi formula) and its relationship with the control surface radius in our accretion calculation, with different number of samples, and different in-grid interpolation techniques. The dashed lines represent 1% and 0.1% error, respectively.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Density slices of the runs with M = 109M⊙ and ﹩{ \mathcal M }=3﹩ at t = 1 Myr (runs A1 to B4), plotted within a region of size 64 pc. The left panel shows the A series, and the right panel shows the B series. Overplotted are density contours and velocity streamlines. Open black circles represent the accretion radius rBHL.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Density, pressure, temperature, and velocity residual profiles of the Bondi test runs, with and without resetting, in comparison with the Bondi solution, taken at t = 1 Myr, around 0.9 of the freefall timescale. Plotted here are runs W0 (blue solid line), P1 (green solid line), W1B (orange solid line), and W1 (red solid line). The temperature calculation assumes a 75% hydrogen/25% helium composition. The overplotted vertical line is the Bondi radius, and the horizontal line represents the ambient value.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Accretion rate and comparison to the predicted Bondi rate for different Bondi test runs plotted as ﹩\dot{M}/{\dot{M}}_{{\rm{B}}}-1﹩. This value equals zero when the measured accretion rate is exactly the same as the predicted value. Top panel: accretion rate with different resetting methods. Plotted here are runs W0 (blue solid line), P1 (green solid line), W1B (orange solid line), and W1 (red solid line). Bottom panel: resetting with a kernel reset for a well-resolved case, but at different accretion and reset radii. Plotted here are W1 (blue), W2 (orange), and W3 (green).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Accretion rate and comparison to the predicted BHL rates of different test runs, for the C series (top) and D series (bottom).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Density slices of the runs with different central black hole masses at t = 1 Myr (runs C1 to C6), plotted within a region of size 64 pc. Open black circles represent the accretion radius rBHL.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Density slices of the runs with different Mach numbers at t = 1 Myr (runs D1 to D4), plotted within a region of size 64 pc. Open black circles represent the accretion radius rBHL.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Accretion rate and comparison to the predicted BHL rates of different test runs, for the A series (top) and B series (bottom).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Left: density and temperature slice plots at t = 1 Myr for runs without reset (left) and with kernel reset (right) in the poorly resolved case (P runs). Right: density and temperature slice plots at t = 1 Myr for runs without reset (left) and with kernel reset (right) for the well-resolved case (W runs).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Density slices at different times for run JA1 with size of control surface Rcs = 4 pc, fixing the jet size at hjet = rjet = 2Δx, where Δx = 0.5 pc. The open white circle represents the control surface radius Rcs.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Comparison of log g estimates obtained by our method with CKS DR2 (left panels, for dwarf stars) and APOGEE DR17 (right panels, for giant stars). The red dashed lines in the top panels are the one-to-one lines. The numbers of stars, mean offset, and dispersion are provided in the lower right corner of each panel. The bottom panels show the residuals in the sense of ﹩\mathrm{log}{g}_{{\rm{phot}}}-\mathrm{log}{g}_{{\rm{APOGEE/CKS}}}﹩, as a function of G magnitude. The red dashed lines in the bottom panels represent the zero level. The golden lines in the bottom panels represent the 1σ scatter. The color bar to the right of each panel codes the number density of stars in the panel.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: The relations between log g−(U − BP)0 and photometric metallicity estimates for main-sequence stars (left panel) and giant stars (right panel). The log g data are from LAMOST DR10, and the metallicities are obtained by our photometric estimates. The numbers of stars are provided in the lower right corner of each panel. The color bar to the right of each panel codes the LAMOST DR10 estimate of log g.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Left panel: an example of the distribution of final photometric estimates of [Fe/H] yielded by the MC simulations. The median value of this distribution is marked by a green dashed line, and the estimate by LAMOST is marked by a red dashed line. Right panel: comparison of the mean uncertainties derived from our MC method with those obtained from APOGEE DR17. The “STD” is estimated by calculating the dispersion of the metallicity difference between photometric method and APOGEE DR17 across various magnitude bins. We use 100 bins, evenly spaced between magnitudes 10 and 16. The red dashed line is the one-to-one line.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Comparisons of stellar mass (left panel) and age (right panel) estimates between this work and SD18 for, respectively, nearly 24,000 main-sequence stars and 14,000 main-sequence turnoff stars in common. The red dashed ine in the left panel is the one-to-one line. In the right panel, the red dashed lines indicate AgeISO = 1.3AgeSD18 and AgeISO = 0.7AgeSD18. The numbers of stars, mean offset, and dispersion are provided in the upper right corner of each panel. The color bar to the right of each panel codes the density number of stars in the panel.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Comparison of Teff obtained by our method with that from CKS DR2 (left panels, for dwarf stars) and APOGEE DR17 (right panels, for giant stars). The red dashed lines in the top panels are the one-to-one lines. The numbers of stars, mean offset, and dispersion are provided in the lower right corner of each panel in the top row. The bottom panels show the residuals in the sense of ﹩{T}_{{\rm{eff}}}^{{\rm{phot}}}-{T}_{{\rm{eff}}}^{{\rm{APOGEE}}}﹩, as a function of G magnitude. The red dashed lines in the bottom panels represent the zero level. The golden lines in the bottom panels represents the 1σ scatter. The color bar to the right of each panel codes the number density of stars in the figure.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Comparison of log g obtained by the isochrone-fitting method with APOGEE DR17 (left panels) and LAMOST DR10 (right panels). The red dashed lines in the top panels are the one-to-one lines. The numbers of stars, mean offset, and dispersion are provided in the upper left corner of each panel in the top row. The bottom panels show the residuals in the sense of ﹩\mathrm{log}{g}_{\,\rm{isochrone fitting}\,}-\mathrm{log}{g}_{{\rm{APOGEE}}/{\rm{LAMOST}}}﹩, as a function of G magnitude. The red dashed lines in the bottom panels represent the zero level. The golden lines in the bottom panels represents the 1σ scatter. The color bar to the right of each panel codes the number density of stars in the panel.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Age distributions for member stars of the four open clusters (NGC 6791, NGC 6811, NGC 6819, and NGC 6866) in the Kepler field. The blue lines represent the ages derived in this work, while the orange lines indicate the ages from SD18. The mean and dispersion of these distributions are marked in the upper right corner of each panel.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: The relations between Teff and color for dwarf stars (including main-sequence stars, turnoff stars, and blue stars, shown in the left panel) and giants (right panel). The Teff data are adopted from LAMOST DR10, and the [Fe/H] data are from our photometric estimates. The numbers of stars are shown in the upper right corner of each panel. The color bar to the right of each panel codes the photometric metallicity estimates.
Paper: Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Authors: Bowen Zhang, Yang Huang, Timothy C. Beers, Kai Xiao, Jifeng Liu, Lei Jia, Henggeng Han, Zhirui Li, Chuanjie Zheng, Yongkang Sun, Ruifeng Shi, Hongrui Gu
Figure caption: Comparisons of surface gravity (left panel), mass (middle panel), and radius (right panel) estimates between this work and CKS. The numbers of stars, mean offset (this work minus CKS), and scatter are marked in the upper left corner of each panel. The red dashed lines are one-to-one lines. The color bar to the right of each panel codes the number density of stars in the panel.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Evolution of accretion rate, shocked volume, and enthalpy for the JC and JD runs.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Figure 12 continued. Left: with fixed resolution and jet radius, varying jet injection height (JC runs). Right: varying the mass of the central black hole and fixing other parameters (JD runs).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Cumulative kinetic energy distribution of entrained material for different runs (JA, JB, JC, and JD).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Evolution of accretion rate for different accretion scenarios (with measuring accretion rate using the Bondi formula or using our flux approach, run J0 vs. JC1 in Table 1), with the same initial condition and jet model. We use a fixed control surface size (Rcs = 2 pc), jet injection region size (hjet = 2 Δx, rjet = 2 Δx), and resolution (Δx = 0.25 pc).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Evolution of accretion rate, shocked volume, and enthalpy for the JA and JB runs.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Gas density in the yz plane at t = 0.2 Myr for the JD runs, with fixed control surface size (Rcs = 2 pc) and resolution (Δx = 0.25 pc) and fixed radius and height of the jet injection cylinder (rjet = hjet = 0.5 pc). The mass of the central black hole varies.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Azimuthally and longitudinally averaged density, pressure, and velocity profiles at t = 0.2 Myr for different jet runs. Left: with varying resolution, where control surface and reset radius are scaled with the resolution (JA runs). Right: fixing resolution and varying jet radius (JB runs).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Gas density slice at t = 0.2 Myr for the JA runs.
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Gas density in the yz plane at t = 0.2 Myr for runs with fixed control surface size and resolution but varying radius and height of the jet injection cylinder. Top panel shows runs varying rjet (JB runs) and bottom panel shows runs varying hjet (JC runs).
Paper: A New Framework for Active Galactic Nucleus Accretion and Jet Feedback in Numerical Simulations
Authors: Ying-He Celeste Lü, 映荷 吕, Paul M. Ricker
Figure caption: Density slices at the same time (t = 0.2 Myr) for runs with different accretion mechanisms (the runs shown are the same as those in Figure 19).
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: Left: Best-fit SFRs for the synthetic population shown in Figure 5 compared to the constant intrinsic SFR of 0.7 × 10−3 M⊙ yr−1. Error bars show the 68% credible intervals. There is very little stellar mass (<0.01 M*) in the most recent time bins (﹩\mathrm{log}\left(\,\rm{age}\,\right)\lt 8﹩), which is why they have larger random uncertainties than older bins. We find good statistical agreement between the input SFRs and those we measure from the synthetic population. Right: same as left, but solved with a lower resolution grid for young stellar populations, resulting in reduced random uncertainties per SFR bin.
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: Left: Cumulative SFHs of WLM measured from the JWST/NIRCAM photometric catalogs of D. R. Weisz et al. (2024) with our methodology (blue) and MATCH (orange, Cohen et al. 2025). The 68% credible interval for our result, considering only random uncertainty, is shaded gray. While there are minor differences, the two results are generally in good agreement. The shaded red region shows the 68% confidence interval for the midpoint of reionization (Planck Collaboration et al. 2020). Right: Solutions for the AMR found with our methodology (blue) and MATCH (orange, Cohen et al. 2025). The slopes are in excellent agreement, with only a minor ∼0.1 dex constant offset. This is likely due to differences in how we model the fixed-age–metallicity distribution.
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: Comparison of WLM data to our best-fit model, formatted for easy comparison to Figure 6(a) of K. B. W. McQuinn et al. (2024) who measured the resolved SFH of WLM with MATCH. (a) Hess diagram of WLM, based on the catalogs of D. R. Weisz et al. (2024) for the full JWST/NIRCAM field of view. (b) Optimal model Hess diagram. (c) Residual between the observed and model Hess diagram in raw star counts. (d) Residual between the observed and model Hess diagram in units of standard deviations (i.e., the residual significance).
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: Results of applying our SFH fitting methodology to the synthetic stellar population shown in Figure 5. The best-fit cumulative SFH (left) and AMR (right) are consistent with those used to construct the synthetic population. The 68% credible intervals, considering only random uncertainties, are shaded in both panels, but this region is too small to see in the right panel.
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: Distribution of the residual significance values from Figure 2(d). If our smooth template were a perfect model, the residual significance values would be normally distributed with mean 0 and standard deviation 1 (shown by the orange line). We achieve a standard deviation of σ ∼ 1, indicating that our model is robust. Our mean is slightly larger as we have excluded bins that are empty in the “observed” Hess diagram for presentational clarity. A normal distribution with these properties is shown in magenta for comparison.
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: The global SFH of WLM measured from the JWST/NIRCam data with our method (blue bars, black error bars) compared to the measurement on the same data with MATCH (Cohen et al. 2025; orange bars, red error bars). Error bars shown are 68% credible intervals considering only random (statistical) uncertainty. Agreement is excellent from the present day to 1 Gyr ago (x = 9) and good from 1 Gyr ago to about 4 Gyr ago (x = 9.6). We see large covariances for time bins from 4 to 6 Gyr ago (x = 9.6–9.8) that result in worse agreement with the MATCH result. We attribute these differences to the significant red clump features present in stellar populations of these ages under our fiducial AMR—the red clump is known to be difficult to model to the level of precision achieved by our data.
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: Analog of Figure 8 for Horologium I. Our best-fit model with [Fe/H] = −2 provides a good fit to the data, but observational constraints on the iron abundance suggest it should have [Fe/H]≤ −2.6. We find the MIST isochrones with such low iron abundances have MSTO colors that are too blue to provide adequate fits. We show 13.65 Gyr isochrones with both [Fe/H] = −2 (blue solid line) and −2.5 (orange dashed line) to illustrate this.
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: Analog of Figure 2 computed with a binary fraction of 70% where binary members are drawn from the IMF for single stars (i.e., independent draws). The same 12.6 Gyr, [M/H] = −2.8 PARSEC isochrone (orange line) and photometric uncertainty and completeness models are used, but the population is modeled at a distance modulus of 17.5 mag (d ≈ 30 kpc). Blue points labeled in panel (a) and overplotted in the other panels indicate stellar masses along the isochrone. The characteristic redward spread of the MS due to the high binary fraction is clearly visible and robustly modeled by the smooth template shown in panel (c).
Paper: Measuring Resolved Star Formation Histories from High-precision Color–Magnitude Diagrams with StarFormationHistories.jl
Authors: Christopher T. Garling, Nitya Kallivayalil, Kristen B. W. McQuinn, Jack T. Warfield, Mario Gennaro, Roger E. Cohen
Figure caption: The CMD, Hess diagram, and optimal model for the synthetic stellar population constructed in Section 3. The properties of the synthetic population (e.g., M* = 107 M⊙, μ = 25 mag) were chosen to roughly emulate WLM.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A1300. A complex cluster with an offset of the mass peak from the X-ray emission peak. An extension in the mass map traces an extension in the X-ray map to the north. WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2345. A chain of three subclusters in a merging system with two relics. WL contours increase in steps of 0.5σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2744. A well-studied, complex system of four subclusters. WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A2163. A low-mass subcluster (W) colliding with a massive primary cluster (E). WL contours increase in steps of 1σ.
Paper: Weak-lensing Characterization of the Dark Matter in 29 Merging Clusters that Exhibit Radio Relics
Authors: Kyle Finner, M. James Jee, Hyejeon Cho, Kim HyeongHan, Wonki Lee, Reinout J. van Weeren, David Wittman, Mijin Yoon
Figure caption: A3411. A merging system with a cool core and a connection between a radio galaxy and radio relic. WL contours increase in steps of 0.5σ. A3412 is detected at the 2.8σ level.