adsabs/AstroCLIMB huggingface dataset:
Paper: The GHOSDT Simulations. II. Missing H2 in Simulations of a Self-regulated Interstellar Medium
Authors: Alon Gurman, Chia-Yu Hu, 家瑜 胡, Michael Y. Grudić, Ulrich P. Steinwandel, Amiel Sternberg
Figure caption: Top panel: normalized mass-weighted density histograms of the total gas mass for simulations in our resolution study, averaged over simulation time 200–500 Myr. The dashed vertical line marks the H I-to-H2 transition density for our m1 model. Bottom panel: mass-weighted density histogram (solid black) and the modified histogram resulting from our subgrid model (dashed black; see Section 4.2), both for model m1. Colored dashed lines show the modified histogram when applied to density bins with a width of 1 dex.
Paper: The GHOSDT Simulations. II. Missing H2 in Simulations of a Self-regulated Interstellar Medium
Authors: Alon Gurman, Chia-Yu Hu, 家瑜 胡, Michael Y. Grudić, Ulrich P. Steinwandel, Amiel Sternberg
Figure caption: Normalized histogram of the total gas mass (violet) and H2 mass (blue) in models m1 (solid lines) and FC-m1 (dashed lines). The black solid and dashed lines show the binned median H2 mass fraction as a function of density for the same models. The shaded regions indicate the density range containing the 25%–75% range of H2 mass in the respective models.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Multifrequency profiles for a pure-H HD 209458 b. The black dashed–dotted line is the original 20 eV monofrequency and pure-H R. A. Murray-Clay et al. (2009) model (﹩{R}_{{\rm{\min }}}=1.037\,{R}_{P}﹩, ﹩\rho ({R}_{{\rm{\min }}})=2.7\times 1{0}^{-11}﹩ g cm, T(﹩{R}_{{\rm{\min }}}﹩) = 1000 K). The gray solid line is also monofrequency 20 eV, but with our updated physical lower BC and bolometric heating and cooling at the base (﹩{R}_{{\rm{\min }}}﹩ = 1.057 RP, ﹩\rho ({R}_{{\rm{\min }}})=1.8\times 1{0}^{-11}﹩ g cm−3, T(R﹩{}_{{\rm{\min }}}﹩) = 1534 K). The remaining plots all use the updated BCs. Purple is the EUV multifrequency (13.6–100 eV) version. Because no metals are present, X-rays (cyan, dashed–dotted, XUV 13.6–2000 eV) contribute relatively little to the profiles or mass-loss rates of a pure-H atmosphere, so the solutions overlie the EUV. Stellar spectra in all simulations are normalized to 450 erg s−1 cm−2 between 13.6 and 40 eV (in keeping with R. A. Murray-Clay et al. 2009). Our model is not valid past the Coriolis radius (upper limit of x-axis). The sonic point and Hill sphere are given by dashed and dotted lines, respectively.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption:  ﹩\dot{M}﹩ and tidal gravity. (a) ﹩\dot{M}﹩ for a planet with parameters of HD 209458 b and a multifrequency XUV, H–He atmosphere is plotted as a function of semimajor axis, a, in au (solid lines) for a high XUV activity, “young” HD 209458 (LXUV ∼ 10−4L*; cyan) and lower XUV flux, older HD 209458 (LXUV ∼ 10−6 L*; orange). Lower/moderate flux is FXUV = 1095 erg s−1 cm−2 and high flux is FXUV = 1.095 × 105 erg s−1 cm−2 at 0.05 au, and the stellar spectral shape does not change. Flux scales with a−2. Traditional energy-limited ﹩\dot{M}﹩ (dotted) and the N. V. Erkaev et al. (2007) tidal-gravity-corrected energy limit ﹩\dot{M}﹩ (dashed) with our modeled efficiencies (average 0.37, computed point by point as described in Section 3.2) are plotted for both flux regimes. (b) Mass loss is plotted as a function of XUV flux. We reproduce Figure 7 of R. A. Murray-Clay et al. (2009; black dashed) for a pure-H, 20 eV monofrequency simulation, in which semimajor axis is held constant while flux at 0.05 au is varied. The ﹩\dot{M}﹩ values are multiplied by the geometric reduction factor of 0.33 for consistency with our current results. The gray line is an update of the previous constant distance line, now with an XUV multifrequency spectrum and a H–He atmosphere. The computed ﹩\dot{M}﹩ values for young and older stars from the left are overplotted. The difference in slope is the result of tidal gravity. We assume that all planets are tidally locked, meaning that we use a constant geometric reduction factor.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Savitzky–Golay smoothed and binned FISM2 solar spectrum scaled to 0.05 au—flux at 0.05 au vs. wavelength in nm (top) and vs. energy in eV (bottom). The solid purple and cyan highlights correspond to the EUV (13.6–100 eV) and X-ray (>100 eV) portions of the spectrum, respectively, and the approximate fluxes of each portion are labeled at the top of the bottom panel in erg s−1 cm−2. Bin edges (thick vertical dashed lines) are automatically set at ionization edges for species present in a given simulation for maximum accuracy in calculating ionization rates (here pure H). Thin vertical dashed lines are the critical points in the smoothing (Appendix E). We crop our spectra in this investigation at 2000 eV because contributions from higher energies are negligible and most photons of energies >2000 eV have τν = 1 surfaces below the base of the wind and do not contribute to driving the wind. The XUV smoothed spectrum for a pure-H planetary atmosphere (above) results in 59 wavelength bins, and the EUV one results in 66.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Energy plot for pure-H XUV versus monofrequency HD 209458 b—energy structure of multifrequency XUV solution (top panel, cyan solution in Figure 4) and 20 eV monofrequency solution (bottom panel, gray solution in Figure 4). The τ(20 eV) = 1 surface for the XUV multispecies is at a higher radius because the deeper penetration of high-energy XUV photons puffs up the atmosphere, resulting in higher densities and optical depths at higher radii than in the monofrequency solution.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Diagram of wind structure. A thermally driven, Parker-wind-like outflow is driven by photoionization heating, primarily deposited near the wind launch radius (R(τXUV) = 1). Our relaxation code solves for the structure of this outflow by integrating between two boundary conditions, the minimum radius of the simulation (﹩{R}_{{\rm{\min }}}﹩) and the sonic point (Rsp), identified by large black crosses. Shorter wavelengths of incident stellar irradiation, like X-rays, are represented by the magenta wave and penetrate deeper into the atmosphere than the longer-wavelength dark purple (higher-energy EUV) and cyan (lower-energy EUV). Magnitude of the local velocity, v, relative to the local sound speed, cs, is given in the middle column. Important planetary radii in the wind’s structure are identified in text in the right column (gray semicircle, RP; thick solid, ﹩{R}_{{\rm{\min }}}﹩; thin solid, RXUV; dashed, Rsp; dotted, RHill; thick solid, Rcori).
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: HD 209458 b multispecies—pure hydrogen (black) and solar abundances of H I, He I, C I, N I, O I, Ne I, and Mg II (green) XUV (11.26–2000 eV) solutions. Vertical lines: sonic points (dashed), Hill radius (dotted), τ(20 eV) = 1 surfaces (light solid); solutions end at the Coriolis radius for each simulation.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Energy deposition fraction for HD 209458 b—fraction of total incident stellar energy into ionizing hydrogen (black), helium (navy), heating (tan), and hydrogen excitation (light green) of which, in our model, 100% is assumed to escape as Lyα radiation. Total XUV flux over 13.6–2000 eV is 1095 erg s−1 cm−2.
Paper: Multilayered Fast Wind Observed in XMM-Newton Snapshot of Seyfert 1 Markarian 877
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, W. N. Brandt, Luigi Gallo, Doyee Byun, Elena Gallo
Figure caption: The outflow momentum rate (﹩{\dot{p}}_{\mathrm{out}}﹩) as a function of the momentum flux of the radiation field (﹩{\dot{p}}_{\mathrm{rad}}﹩). The transparent triangles represent values multiplied by the minimum volume filling factors. The solid and dashed lines are the best-fit lines for the data with unity and minimum volume filling factors. The shaded regions indicate the 1σ confidence level. The best-fit slope m is presented in the legend. The dotted lines marked the equality between ﹩{\dot{p}}_{\mathrm{out}}﹩ and ﹩{\dot{p}}_{\mathrm{rad}}﹩.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: Selenographic distributions of the locations at the lunar surface where fupper is above (a) 1 Hz, (b) 5 Hz, (c) 10 Hz.
Paper: Kinematic Analysis of an Ultrastrong Mg II Absorber at z ≈ 1.13 Linked to Circumgalactic Gas Structures
Authors: Purvi Udhwani, Sameer, Anand Narayanan, Sowgat Muzahid, Jane Charlton, Sebastiano Cantalupo
Figure caption: Top left: white light image from VLT/MUSE with dimensions of ﹩1^{\prime} \times 1^{\prime} ﹩ centered on the quasar Q1621–0042. The quasar light is removed by subtracting the PSF as indicated in Section 2.2. Top right: a narrowband image of the same field centered around the [O II] λλ3726, 3728 doublet at zgal = 1.1334. The [O II] doublet lines are unresolved at the resolution of MUSE. The line of sight to the background quasar Q1621–0042 is indicated with a cross-wire symbol. The circles with dotted lines represent ρ = 50 kpc and ρ = 100 kpc projected separations around the galaxy at zgal. The foreground field of the quasar does not show any other extended source at the redshift of zgal ≈ 1.1334. Bottom: the galaxy spectrum obtained from MUSE is shown in gray. The blue curve is the binned spectrum. The redshifted [O II] emission lines are used to establish the redshift of the galaxy coinciding with the absorber, and determine the SFR of the galaxy.
Paper: Kinematic Analysis of an Ultrastrong Mg II Absorber at z ≈ 1.13 Linked to Circumgalactic Gas Structures
Authors: Purvi Udhwani, Sameer, Anand Narayanan, Sowgat Muzahid, Jane Charlton, Sebastiano Cantalupo
Figure caption: Left: MUSE pseudo-narrowband image spanning the wavelength range 7940–7960 Å centered on the redshifted position of the [O II] λλ3727, 3729 emission. The faint residuals after removing the quasar light are seen at the top left corner of the image. A Gaussian filter of 2σ has also been applied to smoothen the image. Right: the galaxy velocity field map derived using GalPak3D along with the quasar line of sight (white filled circle). The color grid indicates the corresponding velocities in the map. The yellow dotted line represents the major axis of the galaxy at the PA. The concentric ellipsoids define the flux isocontours. The azimuthal angle between the quasar line of sight and the galaxy’s major axis is α ≈ 21﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4. The quasar line of sight probes a region close to the projected major axis where the emitting gas has a velocity of ≈−150 km s−1, tracing the flat part of the rotation curve.
Paper: Kinematic Analysis of an Ultrastrong Mg II Absorber at z ≈ 1.13 Linked to Circumgalactic Gas Structures
Authors: Purvi Udhwani, Sameer, Anand Narayanan, Sowgat Muzahid, Jane Charlton, Sebastiano Cantalupo
Figure caption: The system plot centered on the emission redshift of z = 1.1334 of the nearest galaxy, showing the lines detected at >3σ and their respective Voigt profile fits (red) imposed over the QSO UVES spectra (gray). The colored vertical lines show the different components of each line, with their respective number labeled, used to ascertain the component structure for photoionization modeling. The Mg II profile has 26 components out of which the component structure in the central saturated region is ascertained from the unsaturated Ca II doublet lines, the Fe II multiplets, and the Mg I line. The Fe II λ2586 and Fe II λ2374 lines fall in the Lyα forest region.
Paper: Kinematic Analysis of an Ultrastrong Mg II Absorber at z ≈ 1.13 Linked to Circumgalactic Gas Structures
Authors: Purvi Udhwani, Sameer, Anand Narayanan, Sowgat Muzahid, Jane Charlton, Sebastiano Cantalupo
Figure caption: Ionization properties of the different components contributing to the absorption with corresponding violin plots in the right panel showing posterior distributions for metallicity, hydrogen number density, H I column density, photoionization equilibrium temperature, line-of-sight thickness, and the nonthermal Doppler broadening parameter. The ∗ on the violin plot indicates the median value of the distribution. These posterior distributions reflect only the statistical uncertainties. Columns: (1) velocity of the cloud with respect to the systemic redshift of the galaxy; (2) metallicity of the cloud; (3) total hydrogen number density of the cloud; (4) neutral hydrogen column density of the cloud; (5) temperature of the cloud; (6) inferred line-of-sight thickness of the cloud; (7) nonthermal Doppler broadening parameter of the cloud; (8) thermal Doppler broadening parameter measured for H I; and (9) total Doppler broadening parameter measured for H I.
Paper: Kinematic Analysis of an Ultrastrong Mg II Absorber at z ≈ 1.13 Linked to Circumgalactic Gas Structures
Authors: Purvi Udhwani, Sameer, Anand Narayanan, Sowgat Muzahid, Jane Charlton, Sebastiano Cantalupo
Figure caption: This figure shows the component profiles of metal lines predicted by photoionization models for the 26 components seen in Mg II. The modeling results shown here are summarized in the Appendix.
Paper: Kinematic Analysis of an Ultrastrong Mg II Absorber at z ≈ 1.13 Linked to Circumgalactic Gas Structures
Authors: Purvi Udhwani, Sameer, Anand Narayanan, Sowgat Muzahid, Jane Charlton, Sebastiano Cantalupo
Figure caption: The bottom panel is the projected rotation velocity of the model galaxy Vlos along the line of sight Dlos, based on the corotating disk model given in C. C. Steidel et al. (2002). The model parameters are described in Section 5.2. The top three panels are the primary absorption lines with the blue box highlighting their absorption width and the yellow box highlighting the velocity span covered by the corotating disk model. The 0 km s−1 velocity is at the systemic galactic redshift. As can be seen, only a narrow range of velocities can be explained by a corotating disk–halo structure.
Paper: Kinematic Analysis of an Ultrastrong Mg II Absorber at z ≈ 1.13 Linked to Circumgalactic Gas Structures
Authors: Purvi Udhwani, Sameer, Anand Narayanan, Sowgat Muzahid, Jane Charlton, Sebastiano Cantalupo
Figure caption: Left: the inclination-angle-corrected rotation curve obtained from GalPaK3D. Right: the detected absorption profiles with normalized flux (+ offset) along the x-axis. We exclude all Fe II features except the λ2586 line, as the others are too saturated or have low S/N. This line is also truncated on both sides in the plot due to contamination from the forest, making it visually cleaner for comparison. The dotted lines mark the range of velocities covered by the rotation curve. The central dotted line at 0 km s−1 is for the redshift of the galaxy.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Time-averaged radial profiles of the feedback efficiency ﹩\overline{\eta }(r)﹩ in small-scale simulations (Section 3) with a Bondi radius RB ≈ 400 rg. Runs with different initial conditions are labeled as in Table 2. Solid lines correspond to ground-truth (one-zone) runs, and dashed lines correspond to multizone runs. Black lines indicate simulations (oz, mz) initialized with the nonrotating strongly magnetized B initial conditions (ICs), blue lines indicate weakly magnetized prograde rotating T+ ICs (oz+, mz+), and a red line indicates weakly magnetized retrograde rotating T– ICs (mz-). The cyan (mz+long) and pink (mz-long) lines show the long-term final states of the T+ and T– runs. The vertical dashed gray line marks the location of the Bondi radius RB.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Snapshot of the BH spin a* = 0.9 simulation with Bondi radius RB ≈ 2 × 105 rg (model 2e5 in Table 3), selected at a time when the jet propagates beyond the Bondi radius. The upper and lower rows of panels show slices of the temperature T and density ρ, respectively. The BH spin axis is aligned in the ﹩+\hat{z}﹩-direction. From left to right, the columns go from small to large scales, focusing on the scales relevant to each zone. The relativistic jet extends from the event horizon (≈0.4 mpc for M87*) to beyond ≳5 RB (≳0.3 kpc for M87*), across 6 decades in radius. The scales RB and 5 RB are shown as dashed and dotted circles in the last two columns. The full movie of the simulation can be accessed here: (https://youtu.be/_ecqwibOp4c). We note that the low-density region in the jet might be significantly overestimated due to numerical floors.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Schematics of the multizone method for spinning BH runs with a Bondi radius RB ≈ 2 × 105 rg. The x-axis shows runtime (not to scale), and the y-axis shows radius. Each black box’s vertical extent marks the range of active radii for that zone. Changing colors in the horizontal direction within boxes represent time evolution, while fixed colors outside boxes represent the frozen state of the zone while it is inactive. The figure corresponds to one “V-cycle,” and a complete simulation consists of a large number of these cycles run one after another.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: The total feedback efficiency η (solid lines) and the electromagnetic feedback efficiency ηEM (dashed lines) for different coordinate systems. The black and blue lines (oz+ and mz+) correspond to the uniform polar grid EKS, and the green lines (mz+jks) correspond to the collimating polar grid JKS. While JKS’s high resolution at the poles helps preserve the Poynting flux ηEM to larger distances compared to EKS, the total efficiency η is insensitive to the choice of coordinate system.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Correlation plot of the efficiency η against the shell-averaged angular velocity 〈Ω〉 measured at r = 5 rg. The data correspond to the strongly magnetized one-zone run with B ICs (model oz), and cover one rotation flip episode in the simulation. The color of the dots traces time t divided by the Bondi time tB, with time increasing from purple to yellow.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Snapshots of the electromagnetic energy flux ﹩{T}_{t,{\rm{EM}}}^{r}\sqrt{-g}﹩ at the end of running zone-0 (left panels) and zone-1 (right panels) when using the bflux0 (top panels) and bflux-const (bottom panels) prescriptions. bflux-const preserves the electromagnetic power of the jet across the internal boundary at 8 rg, whereas bflux0 does not.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Dependence of the time-averaged accretion rate ﹩\overline{\dot{M}}﹩ in units of the Bondi rate ﹩{\dot{M}}_{{\rm{B}}}﹩ measured at the BH horizon rH, and the feedback efficiency ﹩\overline{\eta }﹩ measured at RB/3, as a function of the Bondi radius RB for simulations with BH spin a* = 0.9 (filled circles). The accretion rate scales with the Bondi radius as ﹩\bar{\dot{M}}/{\dot{M}}_{{\rm{B}}}\propto {R}_{{\rm{B}}}^{-1/2}﹩, indicated by the blue line. The time-averaged feedback efficiency ﹩\overline{\eta }﹩ is ∼0.3, independent of the Bondi radius RB, and lies between the prograde and retrograde torus feedback efficiency values η = 0.1–1, outlined by the light-green background. For comparison, the spin a* = 0 results using the new multizone setup are shown as unfilled circles for the smallest and largest models (RB ≈ 400, 2 × 105).
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Time evolution of the accretion rate ﹩\dot{M}({r}_{H})﹩ in units of the Bondi accretion rate ﹩{\dot{M}}_{{\rm{B}}}﹩, the feedback efficiency η(5 rg), and the dimensionless magnetic flux parameter ϕb(rH), for four magnetized Bondi simulations with Bondi radii of RB ≈ 400 rg (yellow curves), 2000 rg (red), 2 × 104 rg (purple), and 2 × 105 rg (black). The horizontal bars in corresponding colors indicate the time average of each quantity over the last 20% of the simulation. While the time-averaged accretion rate ﹩\dot{M}﹩ shows a decreasing trend with increasing Bondi radius RB, both the feedback efficiency η and the magnetic flux parameter ϕb remain constant across runs with different Bondi radii.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Time-averaged radial profiles of (left panel) the feedback efficiency ﹩\overline{\eta }﹩, and (right panel) the shell-averaged temperature ﹩\langle \overline{T}\rangle ﹩, for magnetized Bondi accretion with Bondi radii of RB ≈ 400 rg (yellow), ≈2000 rg (red), ≈2 × 104 rg (purple), and ≈2 × 105 rg (black). The vertical dashed lines show the locations of the Bondi radii in corresponding colors. The green band displays the bounds on efficiencies from small-scale torus-like simulations (Figure 2).
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Density profiles averaged over three ranges of the polar angle θ for the 2e5 run with Bondi radius RB ≈ 2 × 105 rg (vertical gray line): north pole (N, red), θ = 0°–30°; south pole (S, blue), θ = 150°–180°; midplane (M, black), θ = 75°–105°. The jet regions (N, S) have a steeper density slope of ρ ∝ r−1.3 compared to the disk region (M) where ρ ∝ r−1.1.