adsabs/AstroCLIMB huggingface dataset:
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: Grid of the resultant 9D, Galactic 3BBF rate (Equation (D1)) distribution, as obtained by Monte Carlo integration with EMCEE (D. Foreman-Mackey et al. 2013), and projected as a set of 2D probability density functions for each dimensional combination. See Table 1 for a description of the independent variables. The sharp discontinuity in the t dimension begins at the onset of star formation in the MW thin disk. This model was generated by fixing the maximum encounter volume to 10% of the local Hill radius (ηH = 0.1, Appendix​​​​​ A.1) and evolving field binaries with the CS prescription (Appendix C.2). The grid was generated using the Python CORNER module (D. Foreman-Mackey 2016).
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: Change of the shape noise with the galaxy image/exposure number in FQ. Dots with different colors show the results from simulations with galaxies of different SNR. The lines are the best-fit linear relations between the square of the shape noise and the inverse of the image number.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: Galaxy–galaxy lensing results. Each column shows results from different lens samples: L1, L2, C1, and C2 from left to right. The upper, middle, and bottom rows show the results of ESD, error of ESD, and ESD_x, respectively. Results from difference bands are labeled with difference colors in every panel. The error bars are estimated with 100 jackknife subsamples. And all the data points are subtracted from the results of the random sample (10 times larger).
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: The results of the field distortion tests with different PSF polynomial orders. The left and right panels show the residuals of g1 and g2, respectively. Lines with the blue, orange, and green colors show the results of the first, second, and third polynomial orders for PSF reconstruction.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: Some statistical properties of our shear catalogs. (a) Distribution of the image number per galaxy; (b) the photo-z distribution; (c) the FWHM distribution of the PSF; (d) the vF distribution. Results of different bands are shown with individual colors in all panels.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: Similar to Figure 9. Results from the official HSC year-one catalog are added.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: Similar to Figure 9, but without the bottom panels for ESD_x. Results from combining the r/i/z bands and all five bands are added.
Paper: Accurate Shear Recovery with Multiband Images of Hyper Suprime-cam
Authors: Cong Liu, Jun Zhang, Hekun Li, Pedro Alonso, Wenting Wang
Figure caption: The sky coverages of the shear catalogs in g/r/i/z/y bands after the cuts.
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: LF of the GC/UCD candidates, plotted as number per 0.2 mag bin in F150W, for MAS0417 (black circles) and Abell 2744 (cyan diamonds). Here the totals per bin are completeness-corrected, and the magnitudes are K-corrected. The MACS0417 bin magnitudes have been shifted by −0.9 mag to put them at the same equivalent distance modulus as Abell 2744, and the numbers are normalized to the same totals at F150W = 29.1 (see text). The solid curves show three log-normal LF models with dispersions σ = 1.2 (red), 1.4 (cyan), and 1.6 (black).
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: The central region of MACS0417, with a color image assembled from the exposures in F090W, F150W, and F200W. In this orientation, north is directed 20° clockwise from vertical, east is left 20° up from horizontal, and the field size shown is approximately ﹩2.{2}^{{\prime} }\,\simeq ﹩ 800 kpc across. Small cyan dots show the point sources with F150W < 29.5 in Zone 1 (see text), while magenta dots show the sources in Zone 2 defined by regions of higher local sky noise. Note the highly elongated spatial distribution around the BCG at the center. The exclusion circle of 50″ described in the text is visible from the distribution of the outer cyan points.
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: Left panel: F150W magnitude vs. local sky noise level for the measured GC candidates. Points are color-coded by recovery probability p(m, σs), with the range of p shown by the colorbar at right. At higher σs, the effective limiting magnitude of the data becomes progressively brighter. The vertical line shows the adopted boundary for dividing the sample into Zones 1 and 2 as discussed in the text. To the left side of the line (Zone 1) the 50% recovery probability is at F150W50 ≃ 29.6. Right panel: F150W measured magnitude vs. recovery probability p(m, σs).
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: Color–magnitude diagrams for the culled sample as described in the text. This sample includes point sources within 50″ of the BCG center to avoid including any parts of the other large galaxies near the edge of the image (at upper right in Figure 3). Measurement uncertainties are indicated by the error bars on the left side of each panel. Objects in Zone 1 are plotted as black symbols, and ones in Zone 2 as red symbols. No adjustments for foreground extinction or K-corrections have been applied for this plot. The dashed lines at F150W ≃29.6 show the approximate 50% recovery probability in Zone 1 (left panel of Figure 2).
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: Distribution of color indices in (F115W − F200W), for point sources in Zone 1 and in the magnitude range 28.0 < F150W < 29.5. The colors are dereddened and a mean K-correction has been applied (see text). A double-Gaussian fit obtained by GMM (see text) to the histogram is shown with blue and red components plotted in the dashed lines and their sum in the solid line. The error bar at middle right shows the expected 1σ spread due to measurement uncertainty at F150W = 29.
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: Upper panel: spatial distribution of the points sources in Zone 1 (low sky level, ﹩{\mathrm{log}}_{10}{\sigma }_{s}\leqslant 3﹩). The (x, y) values are in arcseconds and they are centered on the BCG. The circle has a radius of 50″ = 0.1Rvir. Lower panel: point sources in Zone 2 (high sky level, ﹩{\mathrm{log}}_{10}{\sigma }_{s}\gt 3﹩).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a)–(c) The same as Figure 12 (a)–(c), but enlarged lightcurves of Flare 23. (d) The normalized flare line fluxes, converted from the E.W. values in the panel (c), assuming V-band continuum increase. (e) XMM EPIC-pn and EPIC-MOS1 lightcurves (0.2–12 keV) of Flare 23. The green and pink colored regions corresponds to the Phases 1–10, separated for the spectral analysis. (f)–(h) The spectral analysis results (X-ray luminosity in 0.2–12 keV LX, temperature T, and emission measure EM) of Phases 1–12 of Flare 23, from Table 5.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) The Hα equivalent width values covering Flares 21, 22, and 23 on 2018 October 13 are plotted with red circles, while the normalized OM UVW2 NUV and LCOGT U-band fluxes are plotted with purple and green marks (see Figure 12). (b) Time evolution of the Hα profile from the CHIRON spectra. The vertical axis represents the wavelength, while the gray horizontal dashed lines with velocity values represent the Doppler velocities from the Hα line center. The gray vertical dashed lines indicate the time [1]–time [8], which are shown in (a) (lightcurve) and Figure 15 (spectra). The color map represents the line profile changes from the quiescent profile (see Figure 15(b), (d), (f), and (h)). (c) and (d) Same as panels (a) and (b), but for the Hβ line (see Figure 16). (e) and (f) Same as panels (a) and (b), but for He I D3 5876 Å line and Na I D1 and D2 lines (see Figure 37). (g) and (h) Same as panels (a) and (b), but for the Ca II 8542 Å line (see Figure 38). The excess equivalent width values of Na I D1 and D2 and Ca II 8542 lines are plotted in (e) and (g) (see Figure 12).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Multiwavelength lightcurves of Flares 21–23 on 2018 October 13. (a) and (b) Hα and Hβ equivalent width (E.W.), XMM EPIC-pn X-ray (0.2–12 keV), XMM OM UVW2, LCOGT U-band, SMARTS V-band, and VLA Ku-band lightcurves as in Figure 3. These fluxes and E.W. values are plotted as normalized with the peak and preflare values of Flare 23. The exact flux value is plotted only for the VLA Ku-band radio data. The peak Hα and Hβ E.W. values of Flare 23 are 4.86 Å and 7.97 Å, while the preflare values are 2.45 Å and 1.56 Å, respectively (see Figure 14). (c) The E.W. lightcurves of Hα, Hβ, He I D3 5876 Å, Na I D1 and D2, and Ca II 8542 Å lines from the CHIRON data, as normalized with the peak and preflare values of Flare 23 (as in (a)). The peak He I D3 5876 Å E.W. value of Flare 23 is 1.03 Å, while the preflare value is 0.04 Å (see Figure 14). As for the Na I D1 and D2, and Ca II 8542 Å lines, the E.W. values are measured from the quiescent component subtracted spectra and as the excess equivalent widths (the preflare E.W. values are zero), to identify excess emissions in the line cores of the absorption lines (Figures 37 and 38). The peak Na I D1 and D2, and Ca II 8542 Å excess E.W. values are 0.71 Å and 0.26 Å, respectively (see Figure 14).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: The quiescent phase X-ray spectra of Obs-ID 0822740301 (see Figure 2) with the 10 temperature fit with fixed temperature bins (Table 1). (a), (c), (e), and (g) The data (red circles) and model fits (blue lines) of RGS1, RGS2, PN, and MOS1 are plotted, respectively. Gray points show the wavelength ranges excluded from the fittings (Table 2). The differences between data and model fits are plotted in (b) and (d), and χ = (data − model)/error are plotted in (f) and (h). (i) emission measure (EM) distribution from the fitting. (j) Abundances vs. the first ionization potential (FIP). The FIP values (eV) are from the National Center of Biotechnology Information (https://pubchem.NCBI.nlm.nih.gov/periodic-table/ionization-energy, accessed February 20, 2025).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) Line profiles of the Hα emission line during Flare 22 on 2018 October 13 from the CHIRON spectra. The horizontal and vertical axes represent the wavelength and flux normalized by the continuum. The gray vertical dashed lines with velocity values represent the Doppler velocities from the Hα line center. The red solid and blue dashed lines indicate the line profiles at the time [1] and time [2], respectively, which are indicated in Figures 14(a) and (b) (lightcurve and intensity map) and are during Flare 22. The black dotted line indicates the line profiles in the quiescent phase, which are the average profile during −0.39 to −0.03 hr on this date (see Figure 14(a)). (c), (e), and (g) Same as panel (a), but the line profiles at time [3]–time [8] during Flare 23. (b), (d), (f), and (h) Same as panels (a), (c), (e),and (g), respectively, but the line profile differences from the quiescent phase.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) (1) The quiescent phase RGS2 spectra of the Obs-ID 0822740301 around Ne IX lines in 13.2–14.0 Å and (2) the 10 temperature model fit from Figure 9 (see Table 1, but only Ne abundance (Z(Ne)) is set to zero. (b) (3) The difference between data (1) and model fit (2). (4) Gaussian fit to (3) (see the main text for the details). (c) and (d) Same as (a) and (b) but for the RGS1 spectra O VII lines in 21.4–22.4 Å.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 6, but for the data of 2018 October 24 and 25.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 6, but for the data of 2018 October 21, 22, and 23.
Paper: Cumulative Proton Right-handed Instabilities in the Young Solar Wind Observed by PSP
Authors: Shaaban M. Shaaban, M. Lazar, H. Fichtner, R. A. López, S. Poedts
Figure caption: (Left) Growth rates of the initially pure IIR instability driven by a beam drift velocity ∣vb∣ = 1.1668 vAc for an isotropic beam (Ab = 1, light green), and progressively increasing the beam anisotropy to Ab = 0.35 (black) in steps of 0.05. (Right) Growth rates of the initially pure PFH instability driven by halo anisotropy (Ab = 0.3, light green) for vb = 0, followed by increasing the beam drift velocity to vb = 1.1 vAc (black) in steps of 0.1. The dashed black lines in both panels correspond to the same cumulative case with ∣vb∣ = 1.1668 vAc and Ab = 0.3.
Paper: Cumulative Proton Right-handed Instabilities in the Young Solar Wind Observed by PSP
Authors: Shaaban M. Shaaban, M. Lazar, H. Fichtner, R. A. López, S. Poedts
Figure caption: Effect of the suprathermal Kappa electrons on the maximum growth rate γm/Ωp as a function of Ae (top panel) and the resonant factor of the beam ﹩{\zeta }_{b}^{+}﹩ as a function of ck/ωpp for different values of Ae (bottom panel).
Paper: Cumulative Proton Right-handed Instabilities in the Young Solar Wind Observed by PSP
Authors: Shaaban M. Shaaban, M. Lazar, H. Fichtner, R. A. López, S. Poedts
Figure caption: Effect of the beam drift and the suprathermal Kappa populations in the beam (or halo) on the instability threshold (γm/Ωp = 10−4) as a function of Ab and βc∥.
Paper: Cumulative Proton Right-handed Instabilities in the Young Solar Wind Observed by PSP
Authors: Shaaban M. Shaaban, M. Lazar, H. Fichtner, R. A. López, S. Poedts
Figure caption: Effect of the electron temperature anisotropy Ae ≠ 1 on the instability threshold (γm/Ωp = 10−4) as a function of ∣vb/vAc∣ and βc∥.
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Vertical profiles of density and velocity fields for gas (left) and dust (right) in the saturated state. Velocities are weighted by density and normalized by Πcs. Shaded regions around the curves indicate 1σ temporal variability, and the gray bands mark ±Hp. In the middle two rows, horizontal dashed lines represent spatial and temporal averages from the AB models of B24. The black horizontal dashed line in the bottom panels denotes zero vertical velocity, which holds for unstratified simulations regardless of Π. Gas and dust densities follow Gaussian profiles. Radial velocities for both components peak away from the midplane and deviate from those in B24 at z = 0. Azimuthal velocity profiles resemble the dust density distribution, with midplane values consistent with B24 within the temporal variability. The gas vertical velocity increases approximately linearly with height due to the outflow boundary condition, while the dust exhibits nonzero vertical motion beyond 2Hp but returns back to zero as ρp → 0. However, we caution that altitudes where the magnitude of vz begins to increase from zero are represented by only a tiny fraction of particles, and those at such heights may be sedimenting back toward the midplane without being balanced by diffusion.
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Time evolution of density and velocity dispersions at the midplane in simulations with τs = 0.1 and Z/Π = 0.24. The left and right panels correspond to the gas and dust quantities, respectively. In order from top to bottom, the panels show the dispersions of density and radial, azimuthal, and vertical velocities. Each panel includes an inset to zoom in on the interval t/T = 0–5. Larger Π values result in higher dispersions during the saturated state denoted by the shaded region, except for δρp(z = 0). As shown in the insets, higher Π also results in earlier saturation of the dispersions (but see text for further discussion).
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Time-averaged COM velocities (Equations (10) and (11)) and their vertical gradients as functions of z. The top two panels show the radial component, while the bottom two panels show the azimuthal component. Shaded regions represent 1σ temporal variability, and the gray bands indicate ±Hp. In the first and third panels, horizontal lines mark the COM velocities from B24, where the radial velocity is zero regardless of Π. The dotted curves in the third and bottom panels show the vertical profiles of the corresponding quantities for each Π as predicted by the NSH equilibrium (Equations (12) and (13)); in the bottom panel, the profiles overlap. In our simulations, the radial velocity fluctuates around zero and deviates from the midplane value in B24, showing that vertical gravity redistributes momentum vertically. In contrast, the azimuthal velocity at the midplane closely matches that from B24. The vertical gradients of both velocity components peak near z ≈ ±Hp, with the azimuthal component exhibiting a larger amplitude than the radial component.
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Similar to Figure 8 but for time-averaged midplane dispersions as functions of Π. Black and light blue markers represent the time-averaged values from our simulations and those from B24, respectively. The time averaging is performed over t/T = 10–50 (corresponding to the gray shaded regions in Figure 8) in our simulations and over t/T = 5–10 in the B24 simulations. The dashed lines in each panel (except the top right) represent the best-fit power law (see Equation (15)) to our results and theirs with the resulting k values (i.e., the slope in log-log space) shown in bold text. The figure illustrates that, except for dust density, all quantities scale with Π, and there is a strikingly close match between stratified and unstratified simulations.
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Time-averaged cumulative distribution functions of the midplane dust density (left) and probability density functions of the midplane gas density (right) for models with τs = 0.1 and Z/Π = 0.24 (solid lines). Distributions from B24 are shown as dotted lines. The time averaging is performed over t/T = 10–50 in our models and t/T = 5–10 in the models by B24. Each color corresponds to a different Π value. The dust and gas density fields from both unstratified and stratified simulations exhibit similar trends with Π: the dust density field remains independent of Π, while the gas density distributions become broader as Π increases. Both the unstratified and stratified cases exhibit nearly identical dust density distributions. However, the gas density distribution is broader in the stratified case, especially for Π = 0.1.
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Time evolution of the maximum dust density normalized to the initial midplane gas density (top), dust scale height normalized by ΠH (middle), and midplane dust-to-gas density ratio (bottom) in simulations with τs = 0.1 and Z/Π = 0.24. Given that the maximum density of the Π = 0.01 case increases rapidly after t/T ≈ 50, we restrict our analysis of the saturated state to the range t/T = 10–50, marked by the gray shading. During the state, the time evolution remains similar across these runs, with ϵ ≈ 1, consistent with the unstratified AB models.