adsabs/AstroCLIMB huggingface dataset:
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: After analysis cuts, true redshift distribution for: true SNIa events (blue); true non-SNIa (II+Ib+Ic+Iax+91bg) events (orange); true non-SNIa subset of SN(II+Ib+Ic) (green). WIDE (top) and DEEP (bottom). True non-SNIa events are dominated by SN(II+Ib+Ic) with only one peculiar SNIax; hence, the orange curve is not visible in WIDE, and barely visible for DEEP.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Roman efficiency for zphot SALT3 light curve fits compared to light curve fits using accurate zspec: WIDE (left) and DEEP (right).
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Median fitted color uncertainty (σc) vs. redshift for SN+host zphot (blue) and accurate zspec (orange). The left and right panels show Roman WIDE and DEEP tiers, respectively.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: zHD distribution after BBC stage, for all four subsets as indicated in the legend. zHD is the Hubble diagram redshift: zspec for LSST and zphot for Roman.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Binned distance uncertainty (stat only) from BBC. The redshift-dependent structure is caused by a different sample dominating in each redshift region indicated by the legend.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Second largest SNR after analysis cuts for Roman WIDE and DEEP tiers.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: For analysis of simulations using ΛCDM cosmological parameters ({ΩM, w0, wa} = {0.315, −1, 0}), FoM (horizontal axis) vs. Hubble diagram binning method (vertical axis); ﹩{{ \mathcal C }}_{{\rm{tot}}}﹩ in the blue circle and ﹩{{ \mathcal C }}_{{\rm{stat}}}﹩ in the orange square. The error bar shows the standard deviation among the nine data sets. Panel (a) includes all four tiers. The remaining panels exclude one subsample indicated on the plot.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: BBC-measured contamination (CONTAMBBC) vs. true contamination (CONTAM﹩{}_{{\rm{SIM}}}﹩) for the nine simulated data sets (blue), and for the DES-SN 5YR analysis (orange). The green line shows CONTAMBBC = CONTAM﹩{}_{{\rm{SIM}}}﹩.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: w0-wa contour forecasts (68% and 95% confidence) from analyzing simulated data generated with the standard ΛCDM cosmology in blue ({ΩM, w0, wa} = {0.315, −1, 0}) and the nonstandard cosmology in red ({ΩM, w0, wa} = {0.315, −0.8, −1.0}). To roughly compensate for missing systematics, we show results from the z-binned Hubble diagram that degrades FoM by nearly 40% compared to an unbinned Hubble diagram. Among the nine simulated samples, we show a result for which the best-fit cosmology parameters are close to the true values indicated by the dashed lines.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: For simulations using nonstandard cosmological parameters ({ΩM, w0, wa} = {0.315, − 0.8, −1.0}), FoM (horizontal axis) vs. Hubble diagram binning method (vertical axis); ﹩{{ \mathcal C }}_{{\rm{tot}}}﹩ in the blue circle and ﹩{{ \mathcal C }}_{{\rm{stat}}}﹩ in the orange square. The error bar shows the standard deviation among the nine data sets. Panel (a) includes all four tiers. The remaining panels exclude one subsample indicated on the plot.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: For analysis using ﹩{{ \mathcal C }}_{{\rm{tot}}}﹩, horizontal axis shows the FoM ratio between using nonstandard cosmological parameters ({ΩM, w0, wa} = {0.315, −0.8, −1.0}) and using ΛCDM parameters ({ΩM, w0, wa} = {0.315, −1, 0}); vertical axis shows Hubble diagram binning method. Each set of points connected by lines corresponds to a sample indicated in the legend.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Top panel: BBC fitted distance uncertainty in redshift bins for default SN Ia volumetric rate (blue) and for pessimistic rate (orange); see Figure 2 for volumetric rates vs. redshift. Bottom panel: FoM ratio (all systematics) between pessimistic and default rate, for all sample combinations (legend) and for the 3 Hubble diagram binning methods (vertical axis).
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: dμ/dz vs. true redshift for each Roman tier, and a ΛCDM theory curve in green.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Average bias on wa vs. average bias on w0 for each Hubble diagram binning method. Error bars show the uncertainty on the mean bias. Ideally, the bias values should be consistent with zero.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: FoM (horizontal axis) vs. systematics (vertical axis). The error bar shows the standard deviation among the nine data sets.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Distribution of fitted SALT3 parameters without extended visits (blue) and with extended visits (orange); for t0 (left) and zphot(right). The core component MJD window is 55,000 to 55,725.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Initial abundance plot at 10 GK with neutron degeneracy correction (upper graph) and without neutron degeneracy correction (lower graph).
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Energy generation (beta decay and neutron capture).
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Energy generation.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: zphot distribution for true SNe Ia (blue) and true non-SNIa contamination (orange). The 6 visit cadence is shown above each panel.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Total rate of energy generation, rate of energy generation due to beta decay, and rate of energy generation due to neutron capture with and without neutron degeneracy after 0.019 s.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Temperature and density vs. time.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Neutron capture rates and photodisintegration rates of Mg.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Heavy element abundances with and without neutron degeneracy correction.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Final abundances (with and without neutron degeneracy corrections).
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Abundance plot without neutron degeneracy correction (upper graph) and with neutron degeneracy correction (lower graph).
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Helium abundance.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Electron abundances and neutron abundances with and without neutron correction.
Paper: Degenerate Neutron Capture Rates in the Threshold of Neutron Star–Black Hole Mergers
Authors: Rita K. Y. Lau
Figure caption: Temperature.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Left panel: the temporal and spatial evolution of the l = 1 harmonic mode, 〈C1(r)〉, computed using Equation (15) and normalized by the l = 0 amplitude 〈C0(r)〉. Time is on the x-axis, and the radius from the center of mass, r, is along the y-axis, while the color coding reflects 〈C1(r)〉/〈C0(r)〉, as indicated in the colorbar on the right. The l = 1 mode appears at T ≈ 70 at the center, and the peak amplitude moves outward to a maximum radius of r ≈ 0.4. At late times, the peak 〈C1(r)〉/〈C0(r)〉 settles at r ≈ 0.1. Note the node just below r = 1, where the response is close to zero at all time. Right panel: the temporal evolution of the amplitude of the total gravitational power, Al, computed using Equation (16) and normalized by A0, for different l modes, as indicated. Note how the l = 1 mode starts out growing exponentially with time. The predicted growth rate from linear response theory (see Section 4.4) is indicated by the black dashed line, and is in close agreement with the growth rate in the simulation at early time. At T ∼ 150, though, the A1/A0 value saturates. After a small decline in power, it ultimately reaches a steady state, indicating the saturated mode is long-lived. Note how the A2, A3, A4 values also start growing shortly after A1 grows. This apparent l ≥ 2 power is an artifact from the imperfect representation of the l = 1 mode.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: These figures show the regions in α − γ parameter space, for fixed β, where the system is stable (df/dE < 0 for all E, shaded yellow), unstable (df/dE > 0 at some E but with f(E) ≥ 0 at all E, shaded green), and unphysical (f(E) < 0 at some E, shaded purple). Different panels correspond to three different values of β as indicated. For comparison, some common density profiles are indicated, including the NFW profile (J. F. Navarro et al. 1997) and the modified Hubble (M.H.) profile (J. Binney & S. Tremaine 2008) for β = 3, the perfect sphere (P.S.) profile (T. de Zeeuw 1985), Hernquist (Hern) profile (L. Hernquist 1990), and Jaffe profile (W. Jaffe 1983) for β = 4, and the Plummer (Plum) profile (H. C. Plummer 1911) for β = 5. We also mark our fiducial unstable profile (Fid) that we focus on in this paper. In general, systems become less stable as the transition from the outer to the inner density slopes becomes sharper (larger α). As a consequence, cored systems (small γ) are more susceptible to instability than cusped systems (large γ). The black dashed and white dashed lines show the fitting functions for γstable (Equation (3)) and γphysical (Equation (4)) that mark the stable–unstable and unstable–unphysical boundaries, respectively.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Top panel: frequency diagram plotting Ωϕ vs. Ωr for a random set of 105 particles in the simulation. Each point is color-coded by the maximum range in energy, ﹩{({\rm{\Delta }}E)}_{{\rm{\max }}}={E}_{{\rm{\max }}}-{E}_{{\rm{\min }}}﹩, experienced by the particle over the entire duration of the simulation. Resonances are indicated by the blue lines and labeled by their (lr, lϕ, lp) values. The majority of orbits lie within 1/2 ≤ Ωϕ/Ωr ≤ 1 and have low ﹩{({\rm{\Delta }}E)}_{{\rm{\max }}}﹩. The cusp orbits, i.e., particles that collectively make up the cusp, lie along the resonances and have moderate ﹩{({\rm{\Delta }}E)}_{{\rm{\max }}}﹩ values, as they rapidly circulate about the cusp. The orbits that are close to (but not exactly at) resonances show the largest ﹩{({\rm{\Delta }}E)}_{{\rm{\max }}}﹩ values. These orbits undergo long-period libration, during which their energy oscillates up and down. Bottom panels: orbital energy, E, as a function of time for 10 representative nonresonant (left), near-resonant (center), and cusp (right) orbits.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Left panel: the change in the two-dimensional DF, Δf(E, ℓ), between T = 500 and T = 0. Right panel: the evolution of f(E) (Equation [11]) over time. Note how the bump in f(E) flattens out over time as the l = 1 mode grows. As is evident from the left panel, this erosion of the bump is due to the fact that the phase-space density of particles with E ≳ −0.95 increases, while that of particles with E ≲ −0.95 decreases. As discussed in the text, this involves resonant interactions between the particles and the l = 1 mode. Once the bump has been mostly erased, and ∂f/∂E ∼ 0 at the energies where the inflection used to be, the l = 1 mode saturates, after which there is little to no further evolution in the DF.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Top panel: the trajectory of the cusp in the x–y plane color-coded by time, with the origin fixed at the center of mass and the z-axis pointing along the cusp’s angular momentum vector. Bottom panel: radial distance of the cusp from the center of mass of the system as a function of time. Note how the cusp starts at the center, moves outward as the instability grows, and eventually settles on a moderately eccentric, slowly precessing orbit.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Contours of the dispersion relation ﹩\left|{ \mathcal D }(\omega )\right|﹩ of our fiducial system for the l = 1 harmonic in the complex ω plane. The zero of the ﹩\left|{ \mathcal D }(\omega )\right|﹩ occurs at ωmode = (0.846, 0.042), indicated by the white cross. For comparison, the horizontal green dashed line corresponds to ﹩{\rm{Im}}(\omega )=0.044﹩, which is the linear growth rate of the l = 1 mode inferred from our simulation by fitting the slope of ﹩\mathrm{ln}\left({A}_{1}/{A}_{0}\right)﹩ as a function of time from T = 50 to T = 100, which is in excellent agreement with the growth rate ﹩{\rm{Im}}({\omega }_{{\rm{mod}}})﹩ inferred from linear response theory. The vertical blue dashed line corresponds to Ωp = 0.829, which is the azimuthal frequency of the cusp, inferred from its trajectory. The fact that this is in good agreement with the frequency of the linear mode, ﹩{\rm{Re}}({\omega }_{{\rm{mod}}})﹩, indicates that the mode’s pattern speed undergoes little change as it becomes nonlinear.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Projected over/underdensity (ΔΣ = Σ − Σ0) of our fiducial simulation in the x–y plane. Different panels correspond to snapshots at different time T, as indicated. At T = 70 the signatures of a dipole perturbation begin to emerge, which is clearly visible by T = 100. By T = 150, the l = 1 mode has saturated (see Figure 4), after which the perturbation continues as a long-lived, rotating soliton without any significant sign of a decline in strength.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: The isotropic distribution functions, f(E), for three density profiles with β = 5.0, γ = 0.5, and different values of α, as indicated. As α increases, the system goes from stable (α = 1) to unstable (α = 6) to unphysical (α = 10). The α = 6 profile is our fiducial unstable system that is analyzed in detail in Sections 4 and 5.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Map of the average fractional change in energy, ΔE = E(T) − E0 (color-coded), as a function of time, T, and initial energy E0. The average is computed at each simulation output by averaging ΔE over all particles in small bins of E0. Around T ≈ 100, when the l = 1 starts growing, regions of large positive and negative ΔE appear for E0 ≲ −0.7. The positive and negative ΔE regions are separated by the (0, 1, 1) corotation resonance. There are finer ΔE features at higher E that correspond to higher-order resonances in the system, marked by their (lr, lϕ, lp) values.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Left panel: the average mass of simulation particles as a function of distance from the center of mass at T = 0 (orange) and T = 500 (black dotted) for a simulation of a spherical system with an initial Hernquist density profile. The two lines lie exactly on top of each other, showing that the system experiences no mass segregation, despite the use of a mass spectrum. In other words, the system is collisionless, as required. Right panel: the normalized amplitude of the gravitational power of the l = 1 mode, A1/A0, for simulation runs of our fiducial system with different resolution. Properly resolving the l = 1 mode in the fiducial model requires on the order of 106 particles. With 104 particles, the discreteness noise exceeds the saturation amplitude of the mode, which explains why the simulation reveals no sign of any instability.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: An example of a near-resonant orbit in the simulation. Left panel: trajectory in the inertial frame. Middle panel: trajectory in the frame corotating with the cusp. The red bar indicates the extent of the radial oscillations of the cusp (see Figure 5). Right panel: energy of the particle as a function of time. Note how the particle is tugged back and forth across corotation, resulting in large-amplitude oscillations in its energy. As discussed in the text, the phase mixing among these near-resonant orbits is responsible for eroding the bump in the DF, which in turn causes the saturation of the l = 1 mode.
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: The normalized l = 1 amplitude of the gravitational power, A1/A0, computed with EXP as a function of time. Results are shown for simulations of (α, β, γ) systems with β = 5.0 and γ = 0.5, but different values of α, as indicated. The inset shows the corresponding initial DFs, f(E). As α increases, the depth of the f(E) inflection increases, making the system more unstable. This results in a higher l = 1 saturation amplitude. Note that the system with α = 4 (in red) shows no sign of an instability. As discussed in the text, we suspect that its l = 1 mode is too small to exponentiate above the noise.