adsabs/AstroCLIMB huggingface dataset:
Paper: Effects of Bursty Star Formation on [C II] Line Intensity Mapping of High-redshift Galaxies
Authors: Lun-Jun Liu, Guochao Sun, Tzu-Ching Chang, Steven R. Furlanetto, Charles M. Bradford
Figure caption: Left: comparison of the predicted SFHs, traced by L [CII], with different levels of burstiness controlled by the SFE ϵ ff (0.005, 0.015, and 0.045), for an example halo that grows from M h ≈ 108 M ⊙ at z = 15 to M h ≈ 1011 M ⊙ at z = 5. The thick and thin curves represent SFHs predicted by the bursty (﹩{t}_{{ \mathcal D }}\gt 0﹩) and the equilibrium (﹩{t}_{{ \mathcal D }}=0﹩) models, respectively, with a transition from bursty to steady star formation visible in the former case. Right: contrast between the bursty SFH and the equilibrium SFH for the same example halo in the fiducial bursty star formation model with ϵ ff = 0.015. The differences are represented in terms of the ratio of halo properties, including the [C II] luminosity (black solid), SFR (red dotted), gas mass (blue dashed–dotted), metallicity (green dashed), and stellar mass (yellow solid). The inset shows a zoom-in view of these ratios.
Paper: Effects of Bursty Star Formation on [C II] Line Intensity Mapping of High-redshift Galaxies
Authors: Lun-Jun Liu, Guochao Sun, Tzu-Ching Chang, Steven R. Furlanetto, Charles M. Bradford
Figure caption: The mass and time/redshift dependence of the scatter σ  L  (color code) and the mean of logarithmic [C II] luminosity ﹩\langle \mathrm{log}(L/{L}_{\odot })\rangle ﹩ (overlaid contours) obtained by fitting a log-normal distribution to the predicted L [CII](M h, z) relation of our bursty star formation model. The three panels show results for ϵ ff = 0.005, 0.015, and 0.045, respectively. The growth of σ  L  toward lower halo masses reflects the increasing burstiness of star formation in halos with shallower gravitational potentials, whereas the tilt of the ﹩\langle \mathrm{log}L\rangle ﹩ contours results from the higher growth rate of dark matter halos at earlier times.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Distance between the center of the main cluster to the center of the subcluster plotted as a function of time for different simulations. The initial time is set to the pericenter passage. Top left: Different initial incident angles and different speeds (see Figure 5) for simulations of merger with a gaseous subcluster with mass ratio R = 1:5, and β = 200. Top right: Different mass and gas content in case of a single passage (see Figure 3) for simulations with θ = 30° and v sub  =  2000 km s−1. The dashed lines indicate the gaseous cases while the dotted one indicates the gasless cases. Bottom: Different mass and gas content in case of multiple passages (see Figure 2) for simulations with θ = 20° and v sub = 1380 km s−1. The dashed lines indicate the gaseous cases while the dotted ones indicate the gasless cases.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Some examples of the trajectory of the subcluster around the center of the main cluster (the length of each trajectory varies and is chosen for clarity). Top left: Comparison of different trajectories for different mass ratios, and gas and gasless subclusters. The other initial parameters are set to v sub = 1380 km s−1, and θ = 20°. Top right: Comparison of different mass ratios for the gasless case and θ = 10° (v sub = 1380 km s−1). Bottom left: Comparison of different initial angles for R = 1:10, gasless subcluster. Bottom right: Comparison for different velocities, θ = 30°, R = 1:5, and gaseous subcluster.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Different θ and β. GGM images showing the edges of the SB for simulations of mergers with a gaseous subcluster with mass ratio R = 1:5, initial velocity v sub = 2000 km s−1 and for different values of β = 100, 200, and 1000, and θ = 20°, 30°, and 40°. The dashed line in each panel marks a circle of radius 700 kpc. All images are shown at 7.5 Gyr after the first pericenter passage.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Cold Front Expansion Speed. Plots of the first CF position as a function of time for different simulations, showing the distance traveled by the CF over time. The blue horizontal line indicates the observed position of the ancient CF in Perseus, and the blue area indicates the time span between 6 Gyr and 8.5 Gyr, the time range at which the initial CF in the different simulations reaches the radius of ∼700 kpc.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Different v sub and θ. GGM images for the merger simulations with two different initial velocities (v sub = 1500, 2000 km s−1) and four different angles (θ = 20°, 30°, 40°, 50°). The subcluster is gaseous, the mass ratio is set to R = 1:5 and β = 200. The white dashed line in each panel marks a circle of radius 700 kpc (the distance from the center at which the ancient CF in Perseus is found). All images are shown at 7.5 Gyr after the first pericenter passage.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Different θ and β. Slices of the local β values for simulations with a gaseous subcluster with mass ratio R = 1:5, initial velocity v sub = 2000 km s−1, and for different initial β and θ values. The slices are taking 7.5 Gyr after pericenter passage, in the x y-plane of the simulation (the merger plane) and centered on the potential minimum of the main cluster. Arrows indicate the velocity of the gas particles in both direction and magnitude. All images are shown at 7.5 Gyr after the first pericenter passage.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Different θ and β. GGM maps for simulations of mergers with a gaseous subcluster with mass ratio R = 1:5, initial velocity v sub = 2000 km s−1 and for different values of β = 100, 200, 1000, and θ = 20°, 30°, and 40°. All images are shown at 7.5 Gyr after the first pericenter passage. The split is marked by the white arrow.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Evolution of the split. Projected temperature maps for simulations of mergers with a gaseous subcluster with mass ratio R = 1:5, initial velocity v sub = 2000 km s−1, and for different values of β = 200 and θ = 30°. The time indicated in the bottom right corner of each image is from the first passage. The temperatures are indicated in keV.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: GGM images for different projection angles for the simulation with β = 200, R = 1:5, showing the external edges. All images are shown at 7.5 Gyr after the first pericenter passage.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: The dashed area is the part of the phase space that contributes to the variance of the gradients, after the line-of-sight integration is done through the depth L 2 = L  p  of the c-block. Here, K inj ∼ 1/L inj, while K patch ∼ 1/L  p  and K beam ∼ 1/L  b  > K patch. We see that the wavenumber of relevant modes is dominated by sky component K > k  z , and modes with wavelengths approaching the injection scale (blue shaded region) have little contribution to the gradient variance. Extending the line-of-sight interaction range shrinks the height of the dashed receiver-improving k  z  = 0 approximation.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: Σ parameter for velocity centroids (top row) and synchrotron intensity gradients (bottom row) in strong (left column) and Alfvén (right column) turbulence. The functions are plotted vs. perpendicular ﹩{M}_{{\rm{A}}\perp }={M}_{{\rm{A}}}/\sin \gamma ﹩ argument, for several angles γ between the mean magnetic field and the line of sight, as labeled. Curved thick light blue line corresponds to approximation ﹩{J}_{2}=\exp (-2{M}_{{\rm{A}}}^{2}/{\sin }^{2}\gamma )﹩, while straight thick blue line is its expansion ﹩{J}_{2}\approx 1-2{M}_{{\rm{A}}}^{2}/{\sin }^{2}\gamma ﹩.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: A figure comparing the theoretical expectation (red) to data points from synthetic simulations for velocity centroids with pure Alfvén modes for all four observables as a function of M A. From top left: J 2, p 2, B/T, and Σ2.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: Normalized angular dependence of the 2D spectrum of the gradients as given by Equation (39) (blue, solid) vs. the analytical fit of Equation (40) (red, dashed). Three sets of curves correspond to M A = 0.1, γ = π/2 (the most narrow), M A = 0.1, γ = π/8, and M A = 0.4, γ = π/2 (the widest, which starts showing some deviations of the fit). L  p  = 0.01L inj for all cases.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: Angular dependence of the 2D power spectrum P(ψ  K ) as a function of ψ  K  (recentered with respect to ψ center) in the projected maps from five selected simulation data (huge-0 to huge-4) with only Alfvén modes. Due to the noises of the angular spectrum, the presented curves are the Gaussian fits of the angular spectrum instead of the raw data itself.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption:  J 2 in centroid maps created from synthetic simulations with equal contributions of Alfvén and slow modes as a function of γ. The theoretical approximation in Equation (41) is given by the red dashed line. M A ≈ 0.6 .
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: Two figures showing how the introduction of noises changes the measured J 2 in both synthetic (red) and the Alfvén mode fluctuations of simulation data (blue) at M A = 0.09.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: The variation of Σ2 and its error bars as a function of block size for Alfvén mode centroid at γ = π/2, M A = 0.13.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: (Top): a figure showing how the J 2 parameter computed from both synthetic (green points) and MHD (blue points) simulations are compared to the theoretical prediction in Equation (41) (red dashed line). (Bottom): the Monte Carlo results in estimating the fit on synthetic data on the formula ﹩{J}_{2}=\exp (-{{CM}}^{n})﹩, showing the mean value of n to be ∼2.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: Similar to Equation (8) but with synchrotron intensity gradients. From top left: J 2, p 2, B/T, and Σ2.
Paper: Gradient Technique Theory: Tracing Magnetic Field and Obtaining Magnetic Field Strength
Authors: Alex Lazarian, Ka Ho Yuen, Dmitri Pogosyan
Figure caption: Four panels showing our theoretical prediction (Equation (41)) and its derivatives, (red) relative to the actual numerical results (blue). For J 2, we fit the numerical results with ﹩\exp (-{{CM}}_{{\rm{A}}}^{n})﹩ with the green curve.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Omnidirectional proton VDF for the event on 2001 April 4T14:39:000Z (θ  Bn  = 29.°1 ± 10°, H = 2.15 ± 0.71), with 3 hr intervals denoted by vertical lines (dashed) on either side of the CfA shock time (solid line). On the vertical axis is the angle-averaged VDF, and the time of day is on the horizontal, still with a time interval of ∼184 s. Shown here are 19 representative energy channels of the STICS sensor (legend), from which VDF measurement values were taken and averaged.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Histograms and basic statistics of fitted spectral indices for a subset of events culled from the CfA database and yielded by fitting the time and angle-averaged STICS VDF to model I (top) and model II (bottom). The indices are binned, moreover, by integer values of γ.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Histograms of shock parameters from the entire CfA IP shock database (blue) by Kasper & Stevens, spanning years 1995–2023, and from a subset spanning 1995–2019 inclusive (green). Also shown are the parameter averages μ for both sets. Both forward and reverse shocks are shown, with the inverse of the compression ratio H taken for reverse shocks, yet with the shock-normal angle θ  Bn  unchanged.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Suprathermal proton energy spectra for a shock on 2001 April 4T14:39:000Z, with power law (model I, top panel) and power law with e-folding (model II, bottom panel) fit functions superimposed. Shown are the time-averaged 3D proton VDF upstream (circles) and downstream (crosses) of the shock for each of the six time intervals about the shock passage (−9 hr: black; −6 hr: blue; −3 hr: cyan; +3 hr: green; +6 hr: red; 9 hr: magenta). Also shown are the fit function parameters yielding the plotted curves, obtained by applying the L-M technique to fit the WIND/STICS data.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Fitted spectral normalization constants (f 0) and associated errors with superimposed solar activity (red axes). Errors represent 1σ uncertainties σ  f  given by the L-M method (Equation (7)). sunspot numbers are tabulated in the Solar Bulletin publication by the AAVSO Solar Section. Moreover, the top panels designate upstream (blue, green, cyan) and downstream (red, black, magenta) normalizations obtained with model I (Equation (5)), while the bottom panels show f 0 values for model II (Equation (6)).
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Histograms and basic statistics of fitted rollover energies, given by model II. Here, only rollover energies lying in the STICS range (6.2–223.1 keV/e) are shown, yet the horizontal axis is logarithmic due to the ample diversity of fitted E 0 values within this range.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Histograms and basic statistics (mean μ and standard deviation σ) of fitted VDF leading coefficients or normalization constant f 0, yielded by model I (top) and model II (bottom). The vertical axis here is linear, and the horizontal logarithmic due to the range of values yielded by fitting (f 0 ≃ 0.184–2.41 × 1010 s3 km−6).
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Spectrogram of angle- and time-averaged STICS VDF, for the shock on 2001 April 4T14:39:000Z, showing the “upstream” values at −9 hr (black), −6 hr (blue), and −3 hr (cyan) with respect to the IP shock. Also shown here are the associated errors obtained assuming Poisson statistics.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The tracer distribution in the characteristic 25 M ⊙ model, with red being ejected and blue being bound. The Si and C+O cores are indicated by the solid line for illustration. The top left, top right, bottom left, and bottom right panels stand for four snapshots at equal time steps of ∼4 s, starting from the initial profile.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Statistics of the tracers for the peak temperature ﹩{T}_{\max }﹩ and their corresponding density in the characteristic model S25-1000-1000-15.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The scaled isotope fraction ([X/Fe] ﹩=\,{\mathrm{log}}_{10}({\rm{X}}/﹩Fe)/(X/Fe )⊙) for elements from C to Zn. The two horizontal lines stand for 50% and 200% of the solar value.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The nucleosynthetic yields of the 1D spherical explosion models with the mixing–fallback mechanism to approximate the aspherical yields. Mixing masses of 3–6 M ⊙ are adopted. Top panel: [Fe/O] against [Ne/O]. Middle panel: [Fe/O] against [Ar/O]. Bottom panel: [Fe/O] against [S/O].
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Same as Figure 6, but for the 2D jet-driven SN models presented in this work. Top panel: [Fe/O] against [Ne/O]. Middle panel: [Fe/O] against [Ar/O]. Bottom panel: [Fe/O] against [S/O].
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Same as Figure 1, but for the characteristic model of 20 M ⊙ as the progenitor.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The tracer thermodynamics history for the 25 M ⊙ star assuming spherical (1D; orange squares) and jet-powered (2D; blue circles) explosions.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Top panel: the chemical abundances of Model S20-1000-1000-15 (blue solid line) and its 1D counterpart (red dashed line). Middle panel: same as the top panel, but for Model S25-1000-1000-15 and its 1D counterpart. Bottom panel: same as the top panel, but for Model S40-1000-1000-15 and its 1D counterpart.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Same as Figure 2, but for the 20 and 40 M ⊙ progenitor models with the standard jet.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Chemical abundance patterns of Models S20-1000-1000-15 (20 M ⊙: blue solid line) and S40-1000-1000-15 (40 M ⊙: red dashed line).
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Similar to Figure 1, but for the characteristic model of 40 M ⊙ as the progenitor.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The ejecta mass fraction of the models in Tables 1 and 2.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The ejected 56Ni mass (M 56) against the ejecta mass (M ej) of the jet-driven SN models in this work (20 M ⊙ series: blue circles; 23 M ⊙ series: orange diamonds; 25 M ⊙ series: green triangles; 40 M ⊙ series: green crosses). The plot is overlaid with the observed Type Ib/c SN catalog taken from A. De Cia et al. (2018; brown triangles), F. Taddia et al. (2019; pink squares), and S. Gomez et al. (2022; gray pentagons). The green triangles connected with the line are the spherical explosions of the S25 models with different explosion energies.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The [V/Fe] against [Ti/Fe] relation for the jet-driven SN models in this work. The semitransparent purple diamonds stand for the metal-poor star data taken from I. U. Roederer et al. (2014). The straight line connects the spherical explosion models of S25 with different explosion energies.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The elemental abundances [X/Fe] of our characteristic models using 20 M ⊙ (blue solid line, circle), 25 M ⊙ (green dashed line, triangle), and 40 M ⊙ (red dotted–dashed line, square) models. The two lines correspond to 50% and 200% of the solar value.