adsabs/AstroCLIMB huggingface dataset:
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Time evolutions of the mean (solid curves) and dispersion (dashed curves) of the eccentricities of the planetesimals near 1 au. Left: dependence on the location of the planet. Middle: dependence on the eccentricity of the planet. Right: dependence on the mass of the planet. The dotted lines indicate the forced eccentricities.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Dependence of the time-averaged random velocities of the planetesimals near 1 au on the (a) location, (b) eccentricity, and (c) mass of the planet. The velocities are averaged over ≃25,000 yr.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Similar to Figure 9, but showing the time evolution of the random velocity (velocity dispersion) of the planetesimals near 1 au.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Morphology fractions compared to B/T morphological type selection in EAGLE and FLARES for massive galaxies (M * ≥ 1010  M ⊙). The relative fractions of disks and spheroids are shown as blue squares and red circles, respectively. The blue dotted line shows mean values for galaxies with B/T < 0.75 in EAGLE and FLARES. The dashed line shows galaxies with B/T > 0.75. Shaded regions represents ±2σ for each distribution. The visual classification fractions only account for disks and spheroids to allow a more direct comparison with the two thresholds in B/T in the simulations.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Diagrams showing the evolution of the concentration (C) and asymmetry (A) in four different redshift bins, one for each panel. Peculiars are shown as pink diamonds, disks as blue squares, and spheroids as red circles. The solid lines denote the merger selection threshold on the top, and the late-type/early-type separation on the lower diagonal line. Peculiars display high asymmetries when compared to other types. Disks display late-type-like morphology, while spheroids are regular at lower redshifts, located at the bottom right of the plots, but move toward the center with increasing asymmetry and decreasing concentration with redshift. Galaxies overall get less concentrated and more asymmetric with increasing redshift. However, at high redshifts, sources display higher concentrations and asymmetries when compared to simulations.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Morphology fraction vs. redshift. The evolution of morphology fraction with redshift for the main morphological classes of our classification framework (Figure 2) in two mass bins, ﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })\lt 9﹩ (left) and ﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })\gt 9﹩ (right). Disks, spheroids, and peculiars are shown as blue squares, red circles, and pink diamonds, respectively. The black squares show the disk fractions reported in Ferreira et al. (2023). The white markers show the class fractions before the redshift corrections.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Three examples of the spirality σ  ψ  measurement. The top row shows the standardized images of the sources (q = 1, position angle = 0°) while the bottom row displays the transformation to polar coordinates (r, ϕ) of the above image. Black lines display the gradient field of the image. The σ  ψ  measurement is based on the standard deviation of these field lines. A round shape will show as a horizontal band in the bottom of the image; an elongated component will produce small bends in this distribution, both in the edges and at the center; nonradial asymmetric features will produce very irregular (r, ϕ) distributions, resulting in higher σ  ψ .
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: 2D distributions of log asymmetry (A) vs. log spirality (σ  ψ ) for each class. Distributions of kernel density estimation are shown for the top 50% of each morphological class in five bins of 10% fractions of the distribution. The asymmetry and σ  ψ  correlate strongly, but are independent measurements because each classification distribution has a different slope. Spheroids show high diversity in A and low diversity in σ  ψ , while the contrary is true for disks. These two measurements form a parameter space capable of separating the classes in this sample relatively well compared to C–A.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Fraction of the total stellar mass (f  m ) in each morphology subsample vs. redshift. This represents the relative amount each class contributes to the total stellar mass at that redshift. Disks, spheroids, and peculiars are plotted as blue squares, red circles, and pink diamonds. The contribution from disks shows a trade-off with respect to peculiars and spheroids at higher redshifts. No stellar mass cut is applied: the whole sample is included.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Morphology fractions vs. average specific star formation rate. Disks, spheroids, peculiars, and the other class are plotted as blue squares, red circles, pink diamonds, and gray crosses, respectively. Four redshift bins are shown. For 1.5 < z < 4.5 the disk galaxies dominate the contribution, while for z > 4.5 peculiars contribute similarly or more than disks in each sSFR bin.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Fraction of SFR (f SFR) in each morphology subsample vs. redshift. We show the contribution to total SFR of each redshift bin from each morphological class down to our mass limit. This represents how much each galaxy class contributes to the total SFR at that redshift. Disks, spheroids, and peculiars types are plotted in blue squares, red circles, and pink diamonds, respectively. No stellar mass cut is applied: the whole sample is included.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: Redshift evolution of Sérsic index for each morphology class. Displayed as blue squares, red circles, and pink diamonds are the means for disks, spheroids, and peculiars, respectively. Error bars define the 15% and 85% percentiles of the distributions.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Relative velocities between particles of given mass ratios near 1 au. Each row corresponds to a fixed target mass. The subplots in the left column show the dependence of the relative velocities on the planet mass. Those in the right column show the dependence on the planet eccentricity. In both columns, the dependence on the planet semimajor axis is shown (see legends). The solid curves represent the critical encounter velocity at the weak growth limit given in KW00 for reference. The dashed curves show the growth limit for basalt given in Stewart & Leinhardt (2009). The dotted curves represent the two-body surface escape velocities v esc given in Equation (15).
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Dependence of σ  v  on planet mass M p near 1 au. The σ  v  values are averaged over a time span starting from ≃10,000 yr after the beginning until the end of the simulation (≃20,000 yr in total).
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Distribution of eccentricity vectors near 1 au. The red asterisk marks the forced eccentricity induced by the planet. The “+” signs show the equilibrium locus of the eccentricity vectors. The different colors are for different particle masses as indicated in the legend. The width of the semimajor axis bin is Δa = 0.1  au.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Distributions of the eccentricity (first row), longitude of pericenter (second row), and solid surface density (third row) along the semimajor axis. The four columns represent four equally spaced (roughly) times of evolution: t = 0, t ≃ 10,000, t ≃ 20,000, and t ≃ 30,000 yr. The colors of the dots represent the mass of the particles.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Similar to Figure 5, but showing the dependence of σ  v  on planet semimajor axis a p near 1 au.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Relative velocity between particles of m 1 and m 2 near 1 au for the fiducial model. The velocities are averaged over ≃20,000 yr; the values from the first ≃10,000 yr are skipped to avoid the initially small values due to the initial conditions.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Timescales of gas damping, orbital decay, and secular perturbation near 1 au for the fiducial model. The timescale of secular perturbation is independent of the particle mass.
Paper: Formation of Inner Planets in the Presence of a Cold Jupiter: Orbital Evolution and Relative Velocities of Planetesimals
Authors: Kangrou Guo, Eiichiro Kokubo
Figure caption: Similar to Figure 5, but showing the dependence of σ  v  on planet eccentricity e p near 1 au.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Median GALEX M-dwarf quiescent magnitudes computed from target lightcurves after removing all points flagged as suspect in Section 3.1. The error bars represent the span from the 16th to 84th percentile.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Cumulative probability distributions of local-to-quiescent flux ratios for M0-M2 dwarfs (blue) and M3-M6 dwarfs (green). These are used to estimate the potential number of flares detected by ULTRASAT in both categories. The normal distribution for an S/N = 3 source (set as the threshold of the GALEX sample) is shown in red.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Ratio of numbers of M-dwarfs to G-dwarfs as a function of distance from Earth for galactic latitudes ∣b∣ > 30°.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Comparison of GALEX NUV fluxes obtained from our data reduction with GUVcat as a function of NUV magnitude. GUVcat tends to overestimate fluxes of faint sources for both flaring and non-flaring stars as compared to gPHOTON2.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: (a) GALEX equivalent duration flare frequency distributions and power-law fits for individual spectral types. Plot elements are the same as in Figure 12(a).
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Flare injection recovery simulation results for the power-law fit parameters α and log C. The red curve shows the polynomial fit for the relation between injected and recovered fit parameters. Recovered parameters are shifted from injected values due to exposure gaps inhibiting the complete detection of some flares.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: (a) GALEX energy flare frequency distributions and power-law fits for individual spectral types. Plot elements are the same as in Figure 13(a).
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Example of injection/recovery simulations for a random GALEX source. The green line shows the theoretical detection limit, which matches the start of the recovered detection plateau.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Superposition of all flare profiles in the profile bank.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 340+0
Authors: Yash Bhargava, Sudip Bhattacharyya, Jeroen Homan, Mayukh Pahari
Figure caption: Left: AstroSat/LAXPC (LXP 20) light curve of GX 340+0 in 3–20 keV with 100 s bins. Right: the LXP 20 hardness–intensity diagram (HID) of the source with hard color computed using the background-subtracted count rates in 10–20 keV divided by that in 6–10 keV and intensity represented by the total count rate in 3–20 keV. Representative error bars (minimum and maximum) are shown in gray at the bottom left corner. A part of the Z track (HB and NB) is clearly seen and has been divided into five zones with roughly similar extent on the Z track. Different colors have been used for points corresponding to different zones. The light curve of the left panel is coded with the same colors, which show how the source moved from one zone to another on the Z track.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 340+0
Authors: Yash Bhargava, Sudip Bhattacharyya, Jeroen Homan, Mayukh Pahari
Figure caption: HID zone dependence of key spectral parameters from the XSPEC model tbabs∗(diskbb+bbodyrad+Nthcomp) for the SXT+LAXPC joint modeling of GX 340+0 spectra. The best-fit parameter values corresponding to the disk and blackbody components are shown in the left panels and those of the Comptonizing corona are depicted in the right panels. The total flux depicted in bottom right panel corresponds to the total unabsorbed flux in 3−20 keV. The variation in the blackbody normalization and the complex evolution of the Comptonizing corona lead to the movement of the source along the Z track.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 340+0
Authors: Yash Bhargava, Sudip Bhattacharyya, Jeroen Homan, Mayukh Pahari
Figure caption: Top left: HID zone–resolved spectra for GX 340+0 as extracted from AstroSat SXT (circles) and LAXPC (crosses). The spectra for different HID zones are colored according to the scheme shown in Figure 1. Middle left: the residuals from the best-fit model (Table 1) are shown for each HID zone. Bottom left: ratio of the zone-wise spectra to Zone 3. Right: the XSPEC spectral model tbabs∗(diskbb+bbodyrad+Nthcomp) for best-fit parameter values for zone 2 with various components (see Table 1 for best-fit parameter values and Section 3.2 for more details). For the decomposition plot, the absorption was set to 0.0 to highlight the relative contribution of each component.
Paper: Back to Business: SLX 1746–331 after 13 Years of Silence
Authors: Jing-Qiang Peng, Shu Zhang, Peng-Ju Wang, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Qing-Cang Shui, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Rui-Can Ma, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan, Peng Zhang, Yun-Xiang Xiao, Shu-Jie Zhao
Figure caption: Left panel: evolution of the spectral parameters by the fitting of NICER with M1. N H is the interstellar absorption, T in is the inner disk temperature, Norm(disk) is the normalization of the disk, and F is the flux of the unabsorbed disk from 1 to 100 keV. Right panel: evolution of the spectral parameters by the fitting of Insight-HXMT with M2. T in and Norm(disk) are as before, Γ is the photon index, and Norm(power law) is the normalization of the power-law component.
Paper: Back to Business: SLX 1746–331 after 13 Years of Silence
Authors: Jing-Qiang Peng, Shu Zhang, Peng-Ju Wang, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Qing-Cang Shui, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Rui-Can Ma, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan, Peng Zhang, Yun-Xiang Xiao, Shu-Jie Zhao
Figure caption: The disk unabsorbed flux (1–100 keV) vs. the disk inner temperature (T in). Flux is found to correlate with temperature by being proportional to ﹩{T}_{\mathrm{in}}^{3.98}﹩.
Paper: Back to Business: SLX 1746–331 after 13 Years of Silence
Authors: Jing-Qiang Peng, Shu Zhang, Peng-Ju Wang, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Qing-Cang Shui, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Rui-Can Ma, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan, Peng Zhang, Yun-Xiang Xiao, Shu-Jie Zhao
Figure caption: The relationship between the mass of a black hole and the maximum temperature of the inner disk in the soft state. Left panel: the observed maximum temperature of the inner disk in the soft state. For different maximum temperatures of disks with different outbursts of BH XRBs, we took the mean value. Right panel: estimated temperature of the inner disk at a luminosity of 0.3 L Edd.
Paper: Back to Business: SLX 1746–331 after 13 Years of Silence
Authors: Jing-Qiang Peng, Shu Zhang, Peng-Ju Wang, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Qing-Cang Shui, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Rui-Can Ma, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan, Peng Zhang, Yun-Xiang Xiao, Shu-Jie Zhao
Figure caption: The NICER hardness–intensity diagram of SLX 1746–331, where the hardness is defined as the ratio of 4–10 keV count rate to 1–4 keV count rate. The red arrows represent the direction of the evolution.
Paper: Back to Business: SLX 1746–331 after 13 Years of Silence
Authors: Jing-Qiang Peng, Shu Zhang, Peng-Ju Wang, Shuang-Nan Zhang, Ling-Da Kong, Yu-Peng Chen, Qing-Cang Shui, Long Ji, Jin-Lu Qu, Lian Tao, Ming-Yu Ge, Rui-Can Ma, Zhi Chang, Jian Li, Zhao-sheng Li, Zhuo-Li Yu, Zhe Yan, Peng Zhang, Yun-Xiang Xiao, Shu-Jie Zhao
Figure caption: Light curve of SLX 1764–331 during the 2023 outburst. Top panel: the light curve of Insight-HXMT LE 1–10 keV. Middle panel: the light curve of Insight-HXMT ME 10–30 keV. Bottom panel: the light curve of NICER 1–10 keV.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Figure rotation pattern speeds against rotation durations. For visibility, the durations of DM-only halos have been offset by +0.04 h −1 Gyr. Pattern speeds decrease with longer-lived rotations out to durations of ∼1 h −1 Gyr, beyond which they stabilize. The upper bound of the distribution past 1 h −1 Gyr closely matches the upper stability limit of figure rotation found by Deibel et al. (2011). Completion limits are shown as black dashed lines. The lower completion bound is set by the pattern speed necessary for the principal axes to sweep out an angle greater than the typical uncertainty on the axis orientation, for a given duration. Pattern speeds below the lower completion limit are considered nondetections and are omitted. The upper bound is set by the Nyquist frequency of 90°/snapshot. Short-lived rotations (t  D  ≲ 1h −1 Gyr) can have higher pattern speeds relative to long-lived rotations.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Two-dimensional histograms showing locally averaged timescales for significant evolution of the halo shape as a function of the rotation axis orientation. Timescales are calculated as the halo p/e shape divided by the average time derivative of p/e during the period of rotation. Local averages are calculated using a Gaussian kernel with σ = 6°. In both DM-only and DM + baryon simulations, halos undergoing figure rotation about the minor or major axis have shapes that are stable for greater than one Hubble time, while halos undergoing figure rotation about the intermediate axis have shapes that may change significantly within ∼2h −1 Gyr. For most rotation axis orientations, including those not aligned with any principal axis, DM-only halos have relatively stable shapes, whereas DM + baryon halos rotating about an axis other than the minor or major axis may have their shapes evolve significantly over the duration of the figure rotation.