adsabs/AstroCLIMB huggingface dataset:
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: Schematic illustration of the proposed disk-wind geometry in NGC 4151. The wind exhibits multilayered, asymmetric, and clumpy structures. The continuous disk outflows exhibit a density profile n ∝ r1.5, consistent with BP MHD winds. Close to the central engine, UFOs are primarily magnetohydrodynamically driven due to their high ionization and velocity, while WAs at larger radii are predominantly driven by radiation pressure. The intermediate region containing VFOs likely reflects a transition zone influenced by both radiation and magnetic mechanisms. The dashed lines represent the line of sight to the center engines, passing through the outflowing gas where the absorption features get created. The dotted lines represent the line of sight to the outflowing gas at the far side of the disk, where the emission features get created. The blue and red colors of the line of sight represent blue- and redshifts of the absorption/emission features. As the winds propagate outward, the angle (θ) between the outflow and our line of sight is expected to increase, flattening the observed velocity–ionization slope. Failed winds (represented by downward arrows) indicate clumps of gas that are unable to achieve escape velocity and subsequently fall back onto the disk, producing observed blue emission features.
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: Schematic diagram for the magnetic field topologies outside the black hole, within the poloidal plane. The dashed gray line denotes the location of the equatorial plane. Left: vertical magnetic field across the equatorial plane. Right: radial magnetic field. The hatched square region denotes the area of concentrated matter that predominantly contributes to the synchrotron radiation. The light blue regions near the polar axis indicate the jet regions of quasi-electromagnetic vacuum.
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: Comparison of the ratio z up to the next-to-leading order (Equation (10)) with the exact value under different inflow modes, under a = 0.94 (top) and a = 0.2 (bottom). We have chosen a typical direction for the emitted photons with (λ, η) = (2, 8), and the field line angular velocity is set to ΩB = 0.3ΩH. For results of other parameter choices, see Appendix B.
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: The leading-order net EVPA along the projected event horizon as φ changes, under different spins and inclination angles. We have taken the modulus of χnet to bring it within the range of [−π/2, π/2].
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: Compare the universal relationship of z with the exact z for the plasma under three different flow conditions. The field line angular velocity is set to ΩB = 0.
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: The dashed lines represent the projected event horizons. The circles mark the locations where χ = −π/4, and the triangles mark the locations where χ = π/4. The projection of the black hole’s rotation direction onto the screen aligns with the β-axis.
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: Comparison of the ratio ﹩{ \mathcal A }/{ \mathcal B }﹩ up to the next-to-leading order in Equation (D5) with the exact value for a free-falling plasma under different black hole parameters in the KNTN spacetime, with ΩB = 0 (left) and ΩB = 0.5ΩH (right). We have chosen (a, λ, η) = (0.5, 2, 8).
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: The net EVPA at the event horizon in the images of a Kerr black hole with varying spins, viewed by an on-axis observer. We have taken the modulus of χnet to bring it within the range of [−π/2, π/2].
Paper: Near-horizon Polarization as a Diagnostic of Black Hole Spacetime
Authors: Yehui Hou, Jiewei Huang, Minyong Guo, Yosuke Mizuno, Bin Chen
Figure caption: Compare the universal relationship of z with the exact z for the plasma under three different flow conditions. The field line angular velocity is set to ΩB = 0.5ΩH.
Paper: Atmospheric C/O Ratios of Sub-Neptunes with Magma Oceans: Homemade rather than Inherited
Authors: Aaron Werlen, Caroline Dorn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Molar bulk atmospheric C/O ratio as a function of resulting atmospheric metal mass fraction, Zatm, for all models that include carbon in the metallic phase (from Figure 1). Horizontal dashed lines mark the initial C/O ratios of the disk and the core. The color bar indicates atmospheric mass fraction. Zatm is defined as the mass fraction of all atmospheric constituents except hydrogen, divided by the total atmospheric mass. Circle sizes denote different planetary masses. The left panel shows models with an atmosphere–magma ocean interface (AMOI) temperature of 3000 K and a silicate–metal equilibrium (SME) temperature of 3500 K; the right panel shows models with AMOI temperature of 4000 K and SME temperature of 4500 K. Across all cases, the atmospheric C/O ratio decreases with increasing Zatm, independently of planetary mass.
Paper: Atmospheric C/O Ratios of Sub-Neptunes with Magma Oceans: Homemade rather than Inherited
Authors: Aaron Werlen, Caroline Dorn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Atmospheric structure for a 6 M⊕ and 2.5 R⊕ planet with an atmosphere–magma ocean interface temperature of 3000 K and an equilibrium temperature of ≈600 K. The radius is defined at 1 bar atmospheric pressure. All panels show results for two different eddy diffusion coefficients, Kzz = 104 and 107 cm2s−1, which control vertical mixing in the atmosphere. The stellar spectrum is modeled as a blackbody. The top panel shows the pressure–temperature profile before and after convergence; the middle panel shows the vertical variations in mixing ratios of the dominant carbon- and oxygen-bearing species; and the bottom panel shows the molar atmospheric C/O ratio as a function of pressure. Dashed vertical lines in the bottom panel indicate the initial C/O ratios of the disk and the core, highlighting the distinct C/O ratios of the atmosphere compared to the core and disk. Lower vertical mixing rates lead to stronger vertical gradients in the atmospheric C/O ratio.
Paper: Atmospheric C/O Ratios of Sub-Neptunes with Magma Oceans: Homemade rather than Inherited
Authors: Aaron Werlen, Caroline Dorn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Molar bulk atmospheric C/O ratio as a function of species mixing ratios for the 3000 K atmosphere–magma ocean interface (AMOI) temperature models with carbon in the metallic phase, from Figure 1. Horizontal dashed lines indicate the initial C/O ratios of the disk and the core. P denotes AMOI pressure, which increases with increasing atmospheric C/O ratio. At high atmospheric mass fractions and planetary masses—corresponding to higher pressures—the atmosphere is carbon-rich and CH4-dominated, driving up the C/O ratio. At low atmospheric mass fractions and low pressures, H2O becomes more abundant, and the C/O ratio decreases.
Paper: Atmospheric C/O Ratios of Sub-Neptunes with Magma Oceans: Homemade rather than Inherited
Authors: Aaron Werlen, Caroline Dorn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Molar bulk atmospheric C/O ratio as a function of atmospheric mass fraction. A 6 M⊕ planet with an atmosphere–magma ocean interface (AMOI) temperature of 3000 K and a silicate–metal equilibrium (SME) temperature of 3500 K is shown. The orange dashed line reproduces the default case from Figure 1. Two additional curves illustrate the effect of different carbon partitioning fits from I. Blanchard et al. (2022), spanning the 1σ uncertainty range. Horizontal dashed lines indicate the initial C/O ratios of the disk and the core, with the core value derived from the initial conditions in the C-metal case.
Paper: Atmospheric C/O Ratios of Sub-Neptunes with Magma Oceans: Homemade rather than Inherited
Authors: Aaron Werlen, Caroline Dorn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Same as Figure 5, but showing the effect of varying the silicate–metal equilibrium (SME) temperature. Both curves use the same carbon partitioning fit as in Figure 1. The orange curve corresponds to the default case from Figures 1 and 5, while the blue curve corresponds to an SME temperature of 4000 K. Increasing the SME temperature leads to significantly higher C/O ratios due to enhanced oxygen partitioning into the metal phase.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: The spatial distribution of the final adopted red clump stellar sample in the Galactic cylindrical coordinate with the first row displaying results of LAMOST: the R–Z plane (left) and R–Φ plane (right). The second row presents the corresponding distributions for the APOGEE sample. In both cases, hexbin plots encode stellar number densities via the color bars. These stars exhibit a distribution across the Milky Way spanning the ranges of 7–14 kpc in Galactocentric radial distance R, −5 to 5 kpc in vertical distance from the Galactic plane Z, and −35° to 35° in azimuthal angle Φ. The bottom row shows age (left) and metallicity (right) distributions: black step histograms represent LAMOST, while red traces APOGEE. The final red clump stellar sample encompasses a wide range of ages from 0 to 14 Gyr, and metallicities ranging from −1.5 to +0.5.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: North–south metallicity asymmetries in the outer disk (R > 11 kpc). Panel (a): Median metallicity variations with respect to Z for stellar populations at different azimuthal angles. Panel (b): variations of the metallicity asymmetry (A, see the main text), as a function of ∣Z∣, for stellar populations over −5° < Φ < 15°. The metallicity asymmetries can be found in this panel. Panel (c): variations of metallicity asymmetry A, as a function of ∣Z∣, for stellar populations within −35° < Φ < −5° and 15° < Φ < 35°. The metallicity asymmetries shown in this panel are not significant.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: Comparison of stellar age determinations between LAMOST and APOGEE red clump stars. Left panel: relationship between LAMOST and APOGEE ages derived from the COBS nonparametric regression quantiles. The central 10th, 50th, and 90th percentile intervals are denoted by blue solid and dashed lines, while the polynomial fit is shown as red dashed lines. Right panel: comparison of corrected ages. The violet dashed–dotted line indicates the one-to-one relation. Point densities are encoded by grayscale values according to the color bar on the right.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: The north–south metallicity asymmetry for R > 11 kpc and −5° < Φ < 15° across distinct stellar age groups. Panel (a): metallicity variations, with respect to Z, for different stellar populations. Panel (b): variations of the metallicity asymmetry A, as a function of ∣Z∣, for younger stellar populations. The metallicity asymmetries are found in this panel. Panel (c): variations of the metallicity asymmetry A, as a function of ∣Z∣ for older stellar populations. The metallicity asymmetries shown in this panel are not significant.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: Metallicity-offset distributions of our red clump stellar sample in the R–Z plane across different azimuthal angles. The colors represent the metallicity offsets (the mean metallicity with radial metallicity gradients removed), coded in the color bar to the right. White bins are those containing fewer than three stars.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: Metallicity-offset distributions for various stellar populations of different ages within the azimuthal range of −5° to 15°, as coded in the color bar to the right.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: Upper panel: evolution of W1 − W2. The red dashed line denotes the mean level of the last five epochs. Middle panel: the dust temperature evolution of AT 2019qiz. The red, blue, and green solid lines denote the temperature of astronomical Si, Gra, and SiC, respectively. The dashed lines denote the mean values of the last five epochs. Lower panel: the OUV and IR luminosity evolution of AT 2019qiz. The orange dots denote the OUV blackbody luminosity generated from ZTF and Swift/UVOT data. The red, green, and blue dots denote the IR luminosity assuming dust with a radius of 0.1 μm composed of Si, SiC, and Gra, respectively. The rest-frame days since peak are relative to the date of the optical flare peak (MJD ∼ 58767.61).
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: The multiwavelength light curve of AT 2019qiz. The Swift/UVOT and ZTF photometry is denoted by dots in different colors, and the WISE photometry is denoted by squares. All magnitudes are in the AB magnitude system, except for WISE, which uses the Vega magnitude system.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: The dust luminosity evolution of QPE-associated TDEs AT 2019qiz and AT 2022upj and TDE candidate SDSS J1335+0728. The dust luminosity is derived in the same way as in N. Jiang et al. (2021a), assuming Si grains with a size distribution of N(a) ∝ a−3.5 and taking into account the absorption coefficient. The rest-frame days since peak are relative to the date of the optical flare peak (MJD ∼ 58767.61, ∼59885, and ∼58991, respectively).
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: Comparison of simulated and observed IR light curves of AT 2019qiz. The blue and red dots denote the observational magnitudes of W1 and W2, respectively. The shaded blue and red areas denote the spread of the simulated light curve of the top 1% of the posterior samples with the highest likelihood values.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: The distribution of the Si dust echo model parameters for AT 2019qiz. The values and errors above the plots correspond to the 15.87%, 50%, and 84.13% quantile values of the posterior samples of the parameters, and the black dashed lines show the locations of these values in the plots. The contours in the 2D contour plots reflect the relative numerical density, where darker color means a larger numerical density.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: Schematic picture of the dust echo model. The central SMBH and dusty torus are shown in purple and red, respectively. The dashed parabolas illustrate the isodelay surface at lags of 400, 800, 1200, 1600, and 2000 days, respectively.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: The distributions of original metallicity (the first and third rows) and the subtracted radial mean metallicity (the second and fourth rows) of our red clump stellar sample in the R–Z plane across different azimuthal angles. The colors represent the metallicity, coded in the color bar to the right. White bins are those containing fewer than three stars.
Paper: A North–South Metallicity Asymmetry in the Outer Galactic Disk—Evidence for the Pericentric Passage of the Sagittarius Dwarf Galaxy
Authors: Chun Wang, Yang Huang, Timothy C. Beers, Payel Das, Haibo Yuan, Lizhi Xie, Shi Shao
Figure caption: Similar to Figure 7, but showing results for separate age stellar populations.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: This figure is similar to Figure 5 but with a set of data artificially added at MJD = 60700 for the fitting process, showing the simulated IR light curves. The purple and orange dots denote the hypothetical W1 and W2 data in the decline phase, respectively.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: The WISE light curves of AT 2019qiz. Blue dots: W1 (3.4 μm); red squares: W2 (4.6 μm). The raw single exposures are plotted in light blue and red, while the binned data are plotted in dark blue and red. The red and blue dashed lines denote the average magnitudes at the quiescent phase. The green dashed line marks the time of optical peak.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: This figure is similar to Figure 4 but with a set of IR data artificially added at MJD = 60700 for the fitting process, showing the distributions of the dust echo parameters.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: Similar to Figure 4 but for SiC dust grains, showing the distributions of the dust echo parameters.
Paper: A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
Authors: Mingxin Wu, Ning Jiang, Jiazheng Zhu, Di Luo, Liming Dou, Tinggui Wang
Figure caption: Similar to Figure 4 but for Gra dust grains, showing the distributions of the dust echo parameters.
Paper: VLT/ERIS Observations of the V960 Mon System: A Dust-embedded Substellar Object Formed by Gravitational Instability?
Authors: Anuroop Dasgupta, Alice Zurlo, Philipp Weber, Francesco Maio, Lucas A. Cieza, Davide Fedele, Antonio Garufi, James Miley, Prashant Pathak, Sebastián Pérez, Veronica Roccatagliata
Figure caption: SPHERE/IRDIS H-band (λobs = 1.625 μm) total intensity image of V960 Mon (see P. Weber et al. 2025). The main panel saturates the inner region, to highlight the detection of Source 1 and Source 2, as well as the northern and northeastern components in the H band. Source 3 falls just outside the SPHERE detector. In the H band there are two more point sources visible in this region, which we mark with white circles. Note that the two additional dots east of V960 Mon are detector artifacts. The inset focuses on the inner region on a different scale. Here, sources are marked by black crosses. V960 Mon itself is behind the coronagraph, marked by a purple circle. We want to highlight the detection of the “B” component and especially the nondetection of the ERIS candidate (c) that is at the base of our study.
Paper: VLT/ERIS Observations of the V960 Mon System: A Dust-embedded Substellar Object Formed by Gravitational Instability?
Authors: Anuroop Dasgupta, Alice Zurlo, Philipp Weber, Francesco Maio, Lucas A. Cieza, Davide Fedele, Antonio Garufi, James Miley, Prashant Pathak, Sebastián Pérez, Veronica Roccatagliata
Figure caption: Contrast curve for the total intensity from the SPHERE H band. The vertical dashed line shows the separation of the ﹩{L}^{{\prime} }﹩-band candidate. The gray-shaded area shows the separation covered by the coronagraph.
Paper: VLT/ERIS Observations of the V960 Mon System: A Dust-embedded Substellar Object Formed by Gravitational Instability?
Authors: Anuroop Dasgupta, Alice Zurlo, Philipp Weber, Francesco Maio, Lucas A. Cieza, Davide Fedele, Antonio Garufi, James Miley, Prashant Pathak, Sebastián Pérez, Veronica Roccatagliata
Figure caption: SPHERE/IRDAP polarized light image of V960 Mon in the H band (see P. Weber et al. 2023). The white contours show the ﹩{L}^{{\prime} }﹩ signal. The gray circle delineates the coronagraph used in the observation. The white bars show the AoLP of the polarized light. The inset is at increased contrast and centered on the location of the ERIS candidate, marked by a black cross.
Paper: VLT/ERIS Observations of the V960 Mon System: A Dust-embedded Substellar Object Formed by Gravitational Instability?
Authors: Anuroop Dasgupta, Alice Zurlo, Philipp Weber, Francesco Maio, Lucas A. Cieza, Davide Fedele, Antonio Garufi, James Miley, Prashant Pathak, Sebastián Pérez, Veronica Roccatagliata
Figure caption: VLT/ERIS image of V960 Mon in the ﹩{L}^{{\prime} }﹩ band. The left panel shows the FUor object embedded in its environment, marking the detection of V960 Mon N and V960 Mon NE. The right panel shows a zoom-in onto V960 Mon, overlaid with ALMA Band 6 continuum contours at 3, 4, and 5σrms (see Figure 2 in P. Weber et al. 2023).