adsabs/AstroCLIMB huggingface dataset:
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: The integrated velocity flux contributions from each of the transfers integrated in the range of scales in the inertial range kinertial (gray bands in Figures 17 and 18). All transfers are normalized by the velocity flux of the total transfer function ﹩{{ \mathcal T }}_{uu}^{u}﹩ (last bar), such that the ﹩{{ \mathcal T }}_{uu}^{s}+{{ \mathcal T }}_{uu}^{c}=1﹩ (first two bars) and then the remaining eight transfers, ﹩{{ \mathcal T }}_{cc}^{s}+{{ \mathcal T }}_{cc}^{c}+{{ \mathcal T }}_{ss}^{s}\,+{{ \mathcal T }}_{ss}^{c}+{{ \mathcal T }}_{cs}^{s}+{{ \mathcal T }}_{cs}^{c}+{{ \mathcal T }}_{sc}^{s}+{{ \mathcal T }}_{sc}^{c}=1﹩. The cascade flux ﹩{{ \mathcal T }}_{cc}^{c}﹩ dominates the flux, followed by ﹩{{ \mathcal T }}_{ss}^{s}﹩.
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: The pointwise kinetic helicity ω · u normalized by the rms for a two-dimensional slice along ∇ϕ (left) and perpendicular to ∇ϕ (right). The largest ω · u fluctuations, both in amplitude and size scale, trace the expanding remnants, showing how, even in the absence of global shear and with ﹩{{ \mathcal H }}_{{\rm{kin}}}\approx 0﹩, strong local kinetic helicity fluctuations are generated through detonating SNe.
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: Same as Figure 8, but for mixed-mode shell-to-shell transfers, uc ↔ us, Equations (B1)–(B2).
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: The same as Figure 17, but for mixed-mode cross-scale transfers, uc → us and us → uc.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: Plots of measured median ICCF centroid lags (black circles) as a function of wavelength for each target. All lags are measured with respect to the UVW2 band. The best fits of τ0 with α = 4/3, λ = 1928 Å  to the function ﹩\tau ={\tau }_{0}[{(\lambda /{\lambda }_{0})}^{\alpha }-1]﹩ are shown by the black solid lines. The predictions from the standard thin disk model (Equation (3)) are shown by the black dashed lines.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: Left: Swift UVOT light curves of Fairall 9. Data are ordered by wavelength from the shortest (top) to the longest (bottom). Right: CCFs (in black) and FR/RSS centroid distributions (in color) for each band relative to the UVW2 band. A positive value means the band lags behind UVW2 band.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: The flux–flux diagram of Swift UVOT light curves of Fairall 9. Best-fitting relations are shown as solid lines. Xg indicates the value of X(t) where fλ = 0 for the UVW2 band. Flux–flux relations for other bands evaluated at Xg give the underlying galaxy contribution. Here, we only care about the U band.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: The diffuse continuum ratio spectrum of Fairall 9. The colored curves show the transmission functions of the various Swift/UVOT filters. The black line shows the wavelength dependencies of the diffuse continuum ratio predicted by the CLOUDY simulation for a standard RPC cloud model.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: Left panel: UVW2-band light curves for Fairall 9. Right panel: UVW2-band light curves for NGC 6814. Both panels show the original light curve (blue solid), the long-term trend fit by a second-order (orange dashed), and the detrended light curve (green dotted).
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: The same as Figure 1, but for the second part light curves of Fairall 9.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: The same as Figure 1, but for the first part detrended light curves of Fairall 9.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Time evolution of the azimuthally averaged disk structure of our simulations for different fragmentation velocities (each column corresponds to a particular simulation; see titles). Row (a) shows the evolution of the gas density. Row (b) depicts the evolution of the dust-to-gas ratio. Hatched areas mark regions in which the J. Lim et al. (2024) criterion for strong clumping via the streaming instability is fulfilled. Maximum particle sizes and size distribution power-law exponents are shown in rows (c) and (d), respectively. The thick dashed line marks the location of the planet. Thin dashed lines show the boundaries of the wave-damping zones.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Time evolution of the azimuthally averaged disk structure of our simulations for different α parameters (each column corresponds to a particular simulation; see titles). Row (a) shows the evolution of the gas density. Row (b) depicts the evolution of the dust-to-gas ratio. Hatched areas mark regions in which the J. Lim et al. (2024) criterion for strong clumping via the streaming instability is fulfilled. Maximum particle sizes and size distribution power-law exponents are shown in rows (c) and (d), respectively. The thick dashed line marks the location of the planet. Thin dashed lines show the boundaries of the wave-damping zones.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Concentrations (rows (a), (c), and (e)) and column densities (row (b), (d), and (f)) of dust originating from the outer disk in our simulations with different planetary masses (rows (a) and (b)), fragmentation velocities (rows (c) and (d)), and turbulence parameters (rows (e) and (f)). The thick dashed line marks the location of the planet. Thin dashed lines show the boundaries of the wave-damping zones.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Total mass of dust within the planet’s orbital radius coming from the outer disk (R > 7.8 au) as a function of time for the different simulation runs. The horizontal gray line shows the total dust mass in the inner disk at the beginning of the simulation (∼9 M⊕).
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Average concentration of dust in the inner disk that originates from the outer disk as a function of time for the different simulations presented in this study.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Azimuthally averaged concentration of outer-disk dust (a) and dust size distribution (b) after 45,000 planetary orbits for the low viscosity (α = 2.5 × 10−4) and low fragmentation velocity (vfrag = 50 cm s−1) setup with a planetary mass roughly corresponding to Jupiter’s core (Mp = 0.1MJup = 31.8 M⊕).
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Azimuthally averaged disk profiles for the four simulations with different α parameters after 45,000 orbits (∼533,602 yr) of evolution. Panel (a) shows the radial gas density profiles, and panel (b) depicts the dust density profiles. Maximum particle sizes of the power-law size distributions are shown in panel (c). Thin dashed lines mark the analytically estimated fragmentation limit. The local power-law exponents of the dust size distributions are shown in panel (d).
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Mass of outer-disk dust at the end of the simulations (after 45,000 orbits) as a function of the varied parameters. Power laws are plotted as gray lines to give a rough idea of the scaling and are not fitted to the data.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Global evolution of the grain size distributions (azimuthally averaged) for our simulations with four different planetary masses. Thin dashed lines indicate the boundaries of the radial damping zones. The thick dashed line indicates the location of the planet.
Paper: Constraints on the Progenitor and Explosion of SN 2024ggi in Harmony with Preexplosion Detection and Hydrodynamic Simulations
Authors: Amar Aryan, Erin Higgins, Matt Nicholl, Ting-Wan Chen, Yu-Hsuan Liu
Figure caption: Top, left: the comparison of the bolometric luminosity light curves resulting from the explosion of 10, 11, 12, 13, and 14 M⊙ ZAMS models with SN 2024ggi. Top, right: corresponding photospheric velocity evolution comparisons with the Fe II line velocities of SN 2024ggi. The bolometric light curve and Fe II line velocities have been imported from K. Ertini et al. (2025). The explosions for 14 (with 40% rotation), 15, 16, and 17 M⊙ are not simulated due to their distant position on the HR diagram from the preexplosion-detected progenitor. Middle, left: same as the top left-hand panel but with a steady-state wind CSM included. Middle, right: corresponding photospheric velocity evolution comparisons with the Fe II line velocities of SN 2024ggi. Bottom, left: the comparison of the bolometric luminosity light curves resulting from the explosion of preferred 11 M⊙ model with steady-state wind CSM and also with β-wind CSM. The effect of changing η is also indicated here. Bottom, right: corresponding photospheric velocity evolution comparisons with the Fe II line velocities of SN 2024ggi. All the models here are computed with ﹩{E}_{{\rm{\exp }}}=0.7\,\times \,1{0}^{51}﹩ erg and MNi = 0.049 M⊙ (nicely iterating the nebular phase luminosities as indicated in the insets).
Paper: Constraints on the Progenitor and Explosion of SN 2024ggi in Harmony with Preexplosion Detection and Hydrodynamic Simulations
Authors: Amar Aryan, Erin Higgins, Matt Nicholl, Ting-Wan Chen, Yu-Hsuan Liu
Figure caption: The evolutionary tracks of 10, 11, 12, 13, 14, 15, 16, and 17 M⊙ progenitor models in our simulations. The tracks shown here start from ZAMS and terminate at the pre-SN stages marked by ⋆ for each model. The location of the HST-detected progenitor candidate is also indicated (from D. Xiang et al. 2024). The inset shows our models’ zoomed late stages of evolution.
Paper: Why Do Solar Wind Models Get It Wrong? Understanding the Capabilities of Time-dependent Solar Wind Simulations
Authors: Evangelia Samara, Elena Provornikova, C. Nick Arge, Andrew J. McCubbin, Viacheslav G. Merkin
Figure caption: The same as Figure 10 but for the PSP location. Gaps on the modeling output indicate intervals at which PSP is very close to the inner heliospheric boundary (21.5 Rs).
Paper: Why Do Solar Wind Models Get It Wrong? Understanding the Capabilities of Time-dependent Solar Wind Simulations
Authors: Evangelia Samara, Elena Provornikova, C. Nick Arge, Andrew J. McCubbin, Viacheslav G. Merkin
Figure caption: Example of how DTW is applied between observed and modeled time series at the STEREO-A location between 2021 September 7 and October 6. The green lines show the alignments between the points from one time series that better correspond to the points of the other time series according to DTW. Based on these alignments, histograms of velocity and time differences can be created.
Paper: Constraints on the Progenitor and Explosion of SN 2024ggi in Harmony with Preexplosion Detection and Hydrodynamic Simulations
Authors: Amar Aryan, Erin Higgins, Matt Nicholl, Ting-Wan Chen, Yu-Hsuan Liu
Figure caption: The stellar evolutionary tracks (from ZAMS to pre-SN stage) of 11 M⊙ progenitor models in our simulations, assuming two sets of temporal and spatial resolutions. The models seem to have converged for the chosen temporal and spatial resolutions.
Paper: Why Do Solar Wind Models Get It Wrong? Understanding the Capabilities of Time-dependent Solar Wind Simulations
Authors: Evangelia Samara, Elena Provornikova, C. Nick Arge, Andrew J. McCubbin, Viacheslav G. Merkin
Figure caption: The same as Figure 10 but for the STEREO-A location.
Paper: Why Do Solar Wind Models Get It Wrong? Understanding the Capabilities of Time-dependent Solar Wind Simulations
Authors: Evangelia Samara, Elena Provornikova, C. Nick Arge, Andrew J. McCubbin, Viacheslav G. Merkin
Figure caption: The same as Figure 9 but for the PSP location. Gaps on the modeling output indicate intervals at which PSP is very close to the inner heliospheric boundary (21.5 Rs).
Paper: Why Do Solar Wind Models Get It Wrong? Understanding the Capabilities of Time-dependent Solar Wind Simulations
Authors: Evangelia Samara, Elena Provornikova, C. Nick Arge, Andrew J. McCubbin, Viacheslav G. Merkin
Figure caption: The same as Figure 9 but for the STEREO-A location.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Gas density projection (top) and density-weighted temperature projection (bottom; each projected through a slab of thickness 200 kpc) at z = 7 from the first calibration step, Cal-1 (adiabatic evolution test). We indicate the mean Rvir among the codes (∼7.5 kpc at z = 7) with a black dashed circle. Units are proper kiloparsecs. See Appendix E.2.1 for more information on Cal-1 and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: The z = 7 composite of two-dimensional PDF of density and temperature for the gas within 100 kpc from the center of the main galactic system in the Cal-3 runs (star formation test). The 100 kpc radius sphere encloses the main galaxy, the CGM, and the nearby IGM. A black dashed vertical line marks the density threshold for star formation. See Appendix E.2.3 for more information on Cal-3 and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Gas density projection (top), density-weighted temperature projection (middle), and stellar surface density (bottom) at z = 7 from the third calibration step, Cal-3. The width of each panel is 4Rvir = 30 kpc. The mean Rvir among the codes (∼7.5 kpc) is indicated with a black/white dashed circle. See Appendix E.2.3 for more information on Cal-3 and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Same as Figure 5 but with GADGET-4 and AREPO-TNG. For more information, see Appendix D.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: The z = 7 composite of two-dimensional PDF of density and temperature for the gas within 100 kpc from the center of the main galactic system in the Cal-2 runs (cooling and heating test). The 100 kpc radius sphere encloses the main galaxy, the CGM, and the nearby IGM. A black dashed vertical line is placed at the value of the star formation density threshold (see Section 3.1 of Paper III). See Appendix E.2.2 for more information on Cal-2 and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: The z = 7 composite of probability distribution function (PDF) of density and temperature for the gas within 100 kpc from the center of the main galactic system in the Cal-1 runs. The 100 kpc radius sphere encloses the main galaxy, the circumgalactic medium (CGM), and the nearby intergalactic medium (IGM). Colors represent the total gas mass in each two-dimensional bin. See Appendix E.2.1 for more information on Cal-1 and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Same as Figures 4 and 7 but with GADGET-4 and AREPO-TNG. For more information, see Appendix D.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Similar to Figure 10, but at z = 4.6 (left two panels) and z = 3.5 (right two panels). The gray-shaded region indicates the observational results at z = 3–8 for ﹩{\mathrm{log}}({M}_{\star }/{M}_{\odot })=9.0﹩–9.5 (left) and ﹩{\mathrm{log}}({M}_{\star }/{M}_{\odot })=9.5﹩–10.0 (right) (V. Pandya et al. 2024).
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Same as Figures 2 and 3 but with GADGET-4 and AREPO-TNG.