adsabs/AstroCLIMB huggingface dataset:
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Face-on (top) and edge-on (bottom) disk slice view of the gas density (left row), magnetic field (middle row), and ratio of magnetic energy over turbulent energy, ∼B 2/P turb (right row), at t ∼ 2.5 kyr. The velocity and magnetic field vectors are shown. The width of each panel is 2 × 10−2 pc. The edge-on disk contours are abbreviated by solid black lines and result from a combination of the magnetic support and the surface shock by the accretion flow, as explained in the text.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Edge-on right half-disk slice (direct and left-inverted), as in Figure 4 at t = 2.5 kyr. Left panel: the radial Maxwell stress, T  R ϕ  = −B  R  B  ϕ . Close to the midplane, the negative stress shows the inflow of angular momentum and the mass outflow. Right panel: spherical radial velocity. Close to the disk midplane, the positive radial velocity shows an outflow and/or vortical motion.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Amplification of magnetic field as a function of the spherical radius R. Evolution of B magnitude (top panel), B 2 ∼ ρ −4/3 ratio (middle panel), and P  B /P turb (bottom panel) as a function of spherical radius R, illustrated at five representative times. Note that the R-dependence of the above quantities differs from their dependence in the accretion disk.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: The disk thickness over cylindrical radius, h/r, at t = 2.5 kyr. The red solid line is adopted from Figure 4; the blue dashed line corresponds to c  s /v  c , the dotted line is v A/v  c , and the dashed–dotted line is v  t /v  c , where v  c  is the Keplerian velocity. The disk is supported vertically by the magnetic field between r ∼ 3 × 10−4 pc and 5 × 10−3 pc and by the thermal pressure inside r ∼ 3 × 10−4 pc and is compressed by the accretion flow outside r ∼ 5 × 10−3 pc. All the parameters have been averaged azimuthally and over the disk thickness.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Power spectra of the MHD turbulence at representative times. The Kolmogorov spectrum of energy cascade with the spectrum E(k) ∼ k −5/3 with wavenumber k has been reproduced (not shown) for the inertial range of 10−2 pc−1 ≲ k ≲ 105 pc−1. The spectral energy density profile evolution confirms that E(k) ∼ k 3/2 is injected at largest scales (here ∼100 pc). The turnover happens at later times and progresses to k ∼ 103 pc−1. Formation of the k −3/2 branch at later times is also visible.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Evolution of the profiles of surface density Σ, temperature T, accretion rate ﹩{\dot{M}}_{\mathrm{acc}}﹩, and tangential velocity v  ϕ , as a function of cylindrical radius r in the accumulating accretion disk within r ∼ 0.1 pc, at different times. All the variables have been averaged over the disk thickness, h, and azimuthally.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: The total disk stresses, ﹩{T}_{\theta \phi }^{\mathrm{tot}}﹩ (solid blue line) and ﹩{T}_{R\phi }^{\mathrm{tot}}﹩ (dashed red line), which are the sum of the Maxwell and Reynolds stresses, as a function of z/r at t = 2.5 kyr. The stresses have been calculated at representative r = 5 × 10−4 pc and averaged azimuthally.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: The effective viscosity, α eff (defined in the text), as a function of cylindrical radius r in the accumulating accretion disk in the range of r ∼ 2 × 10−4 pc to 1.0 pc, thus avoiding the core. Parameter α eff has been averaged over disk scale height, h, and azimuthally.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Growth of magnetic radial poloidal B  p  and toroidal B  ϕ  fields as a function of time. Profiles show the fields at cylindrical radius ∼2 × 10−4 pc, ∼5 × 10−4 pc, and ∼2 × 10−3 pc—all values are averaged over the disk thickness, h, and azimuthally.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The comparison between 1D (Model N) and 2D (Model T). The left panels show the evolution of density profiles, and the right panels show the optical depth profiles for band VIII (Model T). The black horizontal lines indicate the photosphere radius. As seen in the right panel, the shock front travels farther in 2D during the same time span, which enlarges the photosphere.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Density and energetics profiles of 1D (Model N) and 2D (Model T) at the peak luminosity. The top panel shows the gas mass density, the middle panel shows radiation flux, and the bottom panel shows the gas energy density. The vertical black lines indicate the photosphere radius for 1D (dotted) and 2D (solid). The locations of the photosphere are ∼7 × 1012 cm in 1D and ∼3 × 1013 cm in 2D. Radiation flux is also larger in 2D. Therefore, the resulting luminosity is ∼1046 erg s−1 in 2D and ∼1045 erg s−1 in 1D.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Density and energetics profiles of 1D (Model N) and 2D (Model T) at the peak luminosity. The top panel shows the gas energy density, the middle panel shows radiation energy density, and the bottom panel shows the ratio of the radiation to gas energies (E rad/E gas) as a function of the normalized radius to the photosphere. The vertical black line shows the location of the photosphere at ξ = 0.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Comparison of 1D and 2D LCs from the viewing angle of 45°. 1D and 2D LCs look different in terms of duration, peak luminosity, and the timing of the peak. Comparing among 2D models, Model P has a lower peak luminosity, and Model R shows stronger fluctuations.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Snapshots of density and velocity of three scenarios at the end of simulations. From left to right, the panel shows Models P, R, and B. The distinct differences in the density and velocity distributions among the three models reflect the impact of the CSM on the shock breakout dynamics that affect the consequent observational signatures.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Color LCs of Model B; the dotted curves are smoothed LCs from data binning. The companion star absorbs and blocks the high-energy photons and then releases the emission of longer wavelengths at 1.25 hr. A double-bump feature appears for longer wavelengths (bands I–IV).
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: The growth of RT fingers during the early phase of shock breakout for Model T with 20482. Panels from left to right show 0.2, 0.3, and 0.4 hr. RT fingers start to emerge and grow in the shocked SN ejecta and CSM.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: LCs of band VIII in Model B. Small fluctuations appear in the rising phase and then soon grow into large variations because of the strong KH and RM instabilities driven by the shock collision with the companion star.
Paper: Multidimensional Radiation Hydrodynamics Simulations of SN 1987A Shock Breakout
Authors: Wun-Yi Chen, Ke-Jung Chen, Masaomi Ono
Figure caption: Density profiles of Model B before and after the shock collision. Due to the shock heating, the companion expands around 25% in size, and the heated envelope of the companion partly escapes through ablation and stripping.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Illustration of the shapes and the orientation of the spots relative to their PA in the ACS/F625W image from 7226 days (2006 December 6). The sizes of the ellipses represent the FWHM of the spots, while the lines originating from the center represent their PA. The bold ellipses in the figure represent hot spots with an orientation uncertainty less than 7.°5, where the uncertainty is one standard deviation of the combined statistical error. The red dashed lines are the unresolved spots and the black solid lines are the resolved spots. The classification of the resolved spots is based on the resolution condition in Equation (1) on the whole data set. Notably, spots 21 and 18 fulfill the resolution condition in the late WFC3 observation.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: The FWHM distribution of stars near SN 1987A, fitted by the 2D Gaussian model (Appendix A). The distributions are categorized based on the instruments used (ACS, WFPC2, and WFC3) and encompass the FWHM of stars fitted across all epochs. The major and minor FWHM were treated as independent in the analysis.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Time evolution of the observed circularized FWHM of all the resolved spots. The error bars here are three standard errors. The red solid line and the shaded region are the average resolution and three standard deviations measured from the star samples for the different instruments. The left is the corresponding physical distances in units of cm, while the right y-axis is in units of mas.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Weighted least square fits of the radial distances of all spots. The residuals shown in the figure are calculated as the weighted difference between the data and the fit, normalized by the uncertainties.
Paper: Temporal Evolution of the Radial Distribution of Milky Way Satellite Galaxies
Authors: Ekta Patel, Lipika Chatur, Yao-Yuan Mao
Figure caption: Left: same as Figure 3 including all satellites with M  V  < –7.5 mag, the magnitude equivalent to the resolution of the Latte simulations. This magnitude selection limits the MW satellite sample to 13–15 satellites, as indicated by the parenthesis in the legend. Middle: same as Figure 3 for all satellites with M  V  < –7.5 mag. The thick black line represents the average R 50 for all Latte MW analogs analyzed in S20. Our results exhibit R 50 values below those of Latte MW analogs, with only minimal overlap with our 2 Gyr ago results. Right: same as the middle panel but only including satellites within 150 kpc. The black vertical line represents the average R 50 for all Latte MW analogs analyzed in S20, also within 150 kpc. Our results for the MW at previous epochs are in good agreement with those from Latte, suggesting the MW may have been more representative of simulated analogs in past evolutionary phases.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Extinction-corrected light curves of SN 2023ufx. The same colors and symbols are used throughout the manuscript. Inverted triangles show 5σ nondetections ∼0.5 days before explosion from ZTF. Blue and red ticks along the lower axis denote optical and NIR spectroscopic observations, respectively. This light-curve information is available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Temporal Evolution of the Radial Distribution of Milky Way Satellite Galaxies
Authors: Ekta Patel, Lipika Chatur, Yao-Yuan Mao
Figure caption: Left: the median distances of all galaxies within 300 kpc of the MW at the present day (D 0) and 1 Gyr ago (D 1). Error bars illustrate the extents of the 25th and 75th percentiles of distance from the 1000 orbits using the Rigid MW+LMC potential described in Section 3.1. Blue stars represent satellites with short orbital periods (P orb ≤ 1 Gyr), yellow diamonds represent satellites with intermediate orbital periods (P orb = 1–2 Gyr), and pink circles represent satellites with long (P orb > 2 Gyr) or unidentified orbital periods. The gray dashed line represents a one-to-one correlation, and the corresponding shaded region encompasses ±15 kpc. Open black squares denote the LMC and the four satellites identified as LMC satellites in Section 4.2. Right: same as the left panel but at 1 Gyr ago (D 1) and 2 Gyr ago (D 2).
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Fe II 5169 Å absorption velocity (top), Hα and Hβ absorption velocities (upper middle), Hα emission FWHM (lower middle), and the pseudo-equivalent width (pEW) ratio of Hα absorption over emission (bottom). The ensemble SN II results of C. P. Gutiérrez et al. (2017a, open circles) are shown in all panels for comparison and the Fe II λ5169 velocities for some well-studied SNe II are included in the top panel. References are provided in Table 5. The information is available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Optical spectra of SN 2023ufx, color coded by instrument and smoothed for visual clarity. Regions with significant telluric or instrumental artifacts are masked. Phases along the right axis are given relative to ﹩{t}_{\exp }﹩ (Section 4.1). These spectra are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Piecewise fits to the r-band fluxes (red, left scale) and the derived L opt (blue, right scale). Colored error bars along the bottom show the estimated transition times between the different phases of light-curve evolution (see Section 4.2).
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Extinction-corrected color evolution of SN 2023ufx compared to other SNe II. Gray vertical lines mark the different stages of evolution (see Section 4.2).
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Preexplosion imaging of the host galaxy from Pan-STARRS. Yellow reticles are 1″ (0.3 kpc) in length and mark the location of SN 2023ufx.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: The velocity anisotropy profiles for halo stars (blue), dark matter particles from TNG300 (yellow) and TNG300-Dark (red), and subhalos from TNG300 (green) and TNG300-Dark (black). Each panel refers to a given mass bin in ﹩{\mathrm{log}}_{10}{{M}}_{200}/{{M}}_{\odot }﹩ (see the text in each panel). The number of subhalos is too few to have good measurements at r < r  s , and this is the reason for the truncation of the green and black curves.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: Relations between the velocity anisotropy parameter and the average virial mass of host dark matter halos (M 200). The red, green, and blue curves are based on halo stars, dark matter particles, and subhalos, respectively. The solid curves are based on objects at outer radii, while the dashed curves are based on objects in more inner regions (see the legend). The error bars are the 1σ scatters of 100 bootstrapped subsamples of galaxies in the same bin of M 200.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: Similar to Figure 4, but we have extended the solid curves in Figure 4 to smaller mass ranges based on TNG50 and TNG100. The curves in this figure are based on halo stars (solid lines), dark matter particles (dashed lines), and subhalos (dotted lines) with r  s  < r < 3 r  s .
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: The velocity anisotropy (β) as a function of the averaged concentration parameter (c 200) of the host dark matter halos, for galaxies in the same bin of host halo virial mass, M 200. Each color curve is based on a given mass bin of M 200, with the legend showing the ranges in ﹩{\mathrm{log}}_{10}{{M}}_{200}/{{M}}_{\odot }﹩. β is calculated using dark matter particles (left), with galactocentric radii of 0.3 r  s  < r < 10 r  s , or halo stars (right), with r  s  < r < 10 r  s , for galaxy systems from TNG300. The error bars are the 1σ scatters of 100 bootstrapped subsamples of galaxy systems.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: Similar to Figure 2, but for dark matter particles from TNG300-Dark.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: Velocity anisotropy profiles for halo stars (top), dark matter particles (middle), and subhalos (bottom), from TNG100 (left) and TNG50 (right). The different color curves refer to different bins in ﹩{\mathrm{log}}_{10}{{M}}_{200}/{{M}}_{\odot }﹩, as indicated by the legend. The error bars are the 1σ scatters of 100 bootstrapped subsamples of galaxy systems in the same mass bin. With the higher-resolution TNG50 and TNG100 simulations, we can push down to smaller M 200 than the results based on TNG300 in previous figures.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: The differences between the velocity anisotropy profiles of halo stars and dark matter particles, for different bins of M 200 (see the legend for the range in ﹩{\mathrm{log}}_{10}{{M}}_{200}/{{M}}_{\odot }﹩).