adsabs/AstroCLIMB huggingface dataset:
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Recovered distributions of eccentricity (e) and MBH spin (χ•) for different true values, demonstrating the regime of applicability of the PN approximation for parameter recovery. Top-left panel: recovered e for true e = 0.7 (green), 0.5 (blue), and 0.3 (red). Top-right panel: recovered e for true a = 100 Rg (red), 50 Rg (blue), and 10 Rg (green). Bottom-left panel: recovered χ• for different values of e (same color scheme as the top-left panel). Bottom-right panel: recovered χ• for different values of a(same color scheme as the top-right panel). Dashed vertical lines mark the true values.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Deviation of 3PN trajectories from the exact Kerr geodesics as a function of Mino time (λ). All trajectories were computed with 10 s time resolution over a 100,000 s baseline.
Paper: On the Eddington Capture Surface around Spherically Symmetric Compact Objects with Separable Luminosity Distributions
Authors: Noah Monk, Adam Rogers
Figure caption: The ECS for the Reissner–Nordström (RN) metric. The compact object is the dark gray disk, and the ECS for a range of RN charge (Q = 0.0 to Q = 0.6) is shown as the light gray annulus, with the Schwarzschild case (Q = 0.0) marked as the dark gray curve on the inner edge. As the RN charge increases, the location of the ECS moves further outward compared to the Schwarzschild case. We launch particles from two positions near the compact object (CO), marked with small open circles. The particles always begin at the location of the Schwarzschild ECS at the ϕ = 0 (three o’clock position on the right-hand side of the CO) and at ϕ = 3π/2 (six o’clock position below the CO). The particles at ϕ = 0 have vanishing radial velocities vr = 0 and initial angular velocities of vϕ = 0.12, vϕ = 0.20, and vϕ = 0.32. The latter particle returns to rest on the ECS at approximately ϕ ≈ π (left-hand side of figure). The inward-traveling particle at ϕ = 3π/2 begins with an initial radial velocity vr = −0.10 and angular velocity vϕ = 0.12. The outward-traveling particle from this position has the same initial conditions except with radial velocity outward vr = 0.10. All quantities are given in normalized units.
Paper: On the Eddington Capture Surface around Spherically Symmetric Compact Objects with Separable Luminosity Distributions
Authors: Noah Monk, Adam Rogers
Figure caption: We use the Schwarzschild metric with R = 5.0 (dimensionless units) and k = 1.50 as in Figure 4. We use the Page luminosity function (Equation (65)) with varying equatorial conductivity χ0. The morphology of the ECS changes as a function of conductivity, becoming more spherical as χ0 approaches unity. Four particles begin at the position of the ECS in the spherical limit, r = rECS ≈ 10.53. The particles above the pole have θ = 0, ϕ = π, and vanishing radial and equatorial velocity (vr = 0, vϕ = 0). The particles above the pole are started with angular velocities vθ = 0, vθ = 0.10, vθ = 0.20, and vθ = 0.30, respectively. The particles to the left of the star are initialized with θ = π/2, ϕ = π, and polar velocities vθ = 0.1 and vθ = 0.01, respectively.
Paper: On the Eddington Capture Surface around Spherically Symmetric Compact Objects with Separable Luminosity Distributions
Authors: Noah Monk, Adam Rogers
Figure caption: ECS for an anisotropic thermally emitting Schwarzschild compact object. We assume the luminosity emitted from the surface follows the surface temperature profile used in the Page model (Equation (65)). The ratio of luminosity at the star’s surface to the Eddington luminosity at maximum is k = 1.50. The Schwarzschild ECS for constant luminosity is given by the solid black line. We use a variety of χ0 values and display the resulting ECS using different line types given in the legend.
Paper: On the Eddington Capture Surface around Spherically Symmetric Compact Objects with Separable Luminosity Distributions
Authors: Noah Monk, Adam Rogers
Figure caption: Examples of asymmetric luminosity distributions giving rise to nonspherical ECSs. Each plot shows an ECS as a cloud of a thousand test particles at rest on the ECS. Here we plot the ECS generated by the spherical harmonics given by ℓ = 3, m = 2 (upper left), ℓ = 4, m = 1 (upper right), ℓ = 6, m = 5 (lower left), and ℓ = 8, m = 0 (lower right). In all plots the star has mass M = 1 and radius R = 5. The ratio of luminosity at the star’s surface to the Eddington luminosity at maximum is k = 1.50. The angular part of the luminosity ranges from a maximum of 1 (light areas on the star) to a minimum of 0.85 (dark areas on the star).
Paper: On the Eddington Capture Surface around Spherically Symmetric Compact Objects with Separable Luminosity Distributions
Authors: Noah Monk, Adam Rogers
Figure caption: The ECS phenomenon around the Schwarzschild–Klinkhamer defect wormhole metric. The dark gray region represents the wormhole, the dark gray curve marks the radius of the Schwarzschild ECS, and the gray annular region marks the ECS for increasing wormhole throat parameter bSK. The particle initial conditions are marked by white disks, with the paths in Schwarzschild spacetime as the solid black curves. The particle trajectories in the wormhole spacetime for throat parameter values of bSK = 2.1, 2.5, and 2.7 are plotted as dashed, dashed–dotted, and dotted lines, respectively. The particle initial conditions are identical to those used in Figure 2.
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: Top panel: Synchrotron intensity Map for simulation M4 overlay with gradient and polarization vector. Color with warmer colors represents stronger intensity. Bottom panel: The AM across different MA.
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: The AM of gradient vs. the block size using synchrotron intensity. The simulation used: M1 Block size covered: [4, 8, 16, 32, 64, 128].
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: Intensity of projected velocity fluctuation (color plot) overlaid with projected magnetic field lines (streamline plot).
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Number of QSOs (left) and QSO F1 scores (right) for the ZTF g-band XGB model based on transformer classifications and median magnitudes as features. We show the results in equally sized and nonoverlapping bins of the number of observations (x-axis) and g-band magnitude (y-axis), where the ticks mark centers of the bins.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Same as Figure 3 but for XGB classification using Astromer classification, ZTF g-band median magnitudes, and WISE features. This model is used for inference in the final catalog.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Transformer classification results on the ZTF g-band data as a function of limiting magnitude and with subsampled time span and number of observation epochs. Each score corresponds to a new training data and model, each training data has the same size, and each light curve within the given training data has the same time span and number of observations. To obtain lower cadences, we sample 100%, 80%, 60%, 40%, 20%, 10%, and 5% of observation epochs, which corresponds to the successive lines on the left plot. Both plots show the same results: left, as a function of time span, and grouped for median cadence, right, as a function of number of observations, and grouped for time span.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Distributions of median g-band magnitude and number of observation epochs for the inference (blue), training (orange), and each class component of the training data (green, red, and purple). The inference and training distributions are normalized to unity, and the class distributions are normalized to one-third.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Number of quasars available in the training sample (blue), and their crossmatches with PS (orange), WISE (green), and Gaia (red). The vertical line shows the ZTF’s magnitude limit, while for the other surveys, we apply limiting magnitude cuts as described in Section 2.4. We note that the final catalog has no magnitude cuts on the WISE survey.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Feature importance from XGB models trained on binary QSO vs. non-QSO classification problem, using the ZTF g-band data with included features from the other surveys. Top: ZTF training sample and processing of missing features, bottom: subsample of objects detected by every survey, with all the features present. plc (QSO) stands for the ZTF light-curve-based QSO classification probability.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: QSO F1 scores for the XGB g-band models trained on the ZTF × PS data, as functions of median magnitude (top left), mean magnitude error (top right), number of ZTF observation epochs (bottom left), and SDSS spectroscopic redshift (bottom right). The gray dashed lines show overlaid quasar distributions. The models are trained using combinations of ZTF transformer classification, ZTF magnitude, and PS griz magnitudes and colors.
Paper: The Frequency-independent Radio Luminosity–Orbital/Rotational Period Relation of RS CVn Stars
Authors: Qichen Huang, 启宸 黄, Biwei Jiang,  碧 沩 姜
Figure caption: (a) Upper panel: maximum radio luminosity–rotation period correlation, where circles represent sources from SRSC and black triangles represent sources from S. Toet et al. (2021). The red solid line (LF-Thiswork) represents the linear fit to 42 RS CVn stars in our work, and the blue solid line (LF-Toet+2021) represents the linear fit to 54 RS CVns, which included 12 sources from S. Toet et al. (2021). The dashed lines of each color indicate the 1.5σ confidence intervals of the fit. The Pearson correlation coefficient (PCC) of both 42/54 sources is listed in the upper left. The value of P indicates the probability of observing a PCC value equal to the calculated result, under the null hypothesis that there is truly no linear correlation between the two variables in the population. Lower panel: maximum radio luminosity–rotation period correlation for all 54 sources, with observations from 144 to 3000 MHz represented by different colors and shapes. The meanings of solid and dashed lines are the same as those in the upper panel. (b) The distribution of PCC between orbital period and radio luminosity derived from 1000 sets of MCMC simulations, with the red dashed line indicating the PCC value of 0.698 calculated from our 42 sources.
Paper: The Frequency-independent Radio Luminosity–Orbital/Rotational Period Relation of RS CVn Stars
Authors: Qichen Huang, 启宸 黄, Biwei Jiang,  碧 沩 姜
Figure caption: (a) Relationship between stellar mass and maximum radio luminosity. Red triangles denote secondary stars, blue circles primary stars, and yellow squares total binary mass. Colored dashed lines show linear fits for each mass category. (b) Relationship between Rossby number (activity indicator) and maximum radio luminosity, with color coding indicating stellar mass. The dashed line at Ro = 0.13 marks the stellar activity boundary. (c) Relationship between binary semimajor axis and maximum radio luminosity. Circles represent SRSC sources, triangles denote sources from S. Toet et al. (2021), with colors indicating primary star mass.
Paper: The Frequency-independent Radio Luminosity–Orbital/Rotational Period Relation of RS CVn Stars
Authors: Qichen Huang, 启宸 黄, Biwei Jiang,  碧 沩 姜
Figure caption: Light curves for (a) TIC 42705187 (2.13 day period) and (b) TIC 28619091 (4.9 day period). For each source, the upper panels show original light curves; the lower panels display results after periodic signal removal (the strongest signal removed iteratively four times for (a), once for (b)). The left panels present time-series data; the right panels show phase-folded results. Eclipse depth measurements used the lower-right panel for (a) and the lower-left panel for (b).
Paper: The Frequency-independent Radio Luminosity–Orbital/Rotational Period Relation of RS CVn Stars
Authors: Qichen Huang, 启宸 黄, Biwei Jiang,  碧 沩 姜
Figure caption: A total of 60 RS CVn stars placed in a Gaia third data release (DR3) color–magnitude diagram. Gray points are 2 minute cadence observation targets of TESS sectors 1 and 2, which are also contained in Gaia DR3. All distance data were provided by C. A. L. Bailer-Jones et al. (2021). Colors indicated the maximum radio luminosity of RS CVn stars.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Time evolution of an initially mono-energetic stellar population with initial half-light radius rh0/rmx0 = 1/64, deeply embedded in a cuspy (left) and a cored (right) dark matter halo. The dark matter mass sourcing the potential is lowered impulsively so that both stellar tracers expand by a factor of roughly 2 with respect to their initial half-light radius. Top row: evolution of the half-light radius as a function of time. The 25th and 75th percentiles of the stellar radial distributions are enclosed by the gray shaded band. Times are expressed in units of the period Th0 of a circular orbit at the half-light radius at t = 0. Second row: average velocity dispersion 〈σ2〉. The radial and tangential components are shown separately as gray and yellow curves, respectively. Third row: virial quantities. total kinetic energy T, total potential energy W, and their sum 2K + W. Fourth row: ratio of mass Mh enclosed within the half-light radius and dynamically estimated mass Mest = rh〈σ2〉/G. Bottom row: half-light radius and velocity dispersion, normalized to their initial values. While the stellar model embedded in the cuspy halo rapidly phase mixes toward an equilibrium configuration, the stellar population embedded in the cored halo undoes several damped oscillations (in energy, size, and velocity dispersion) before reaching a phase-mixed equilibrium state. For videos supplementing this figure, see Appendix C.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Like Figure 7, but showing the equilibrium energy distributions of four stellar tracers reached after an impulsive change to the underlying potential. Energies are expressed relative to the initial potential minimum. In contrast to the adiabatic case, here the stellar energy distributions widen considerably when the potential changes. These widening distributions may overlap, energetically mixing the stellar populations. Stars are lost once the stellar energy distributions extend into unbound states (gray area with ﹩{{ \mathcal E }}^{({\rm{IC}})}\geqslant 1﹩). The bottom panel shows the energy distributions measured in the simulation with M/M0 = 1/10 in units of the evolved potential minimum. Dotted black curves show the energy distributions expected from the conservation of single-particle energies ﹩{ \mathcal E }={u}^{2}/2+\psi (r)﹩ in the evolved potential (see Equation (40)). See Figure 18 for a version of this plot that includes the case of impulsive deepening of the underlying potential.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Left panels: number density profile ν⋆(r) (top) and anisotropy ﹩\beta (r)=1-{\sigma }_{{\rm{t}}}^{2}/(2{\sigma }_{{\rm{r}}}^{2})﹩ (bottom) of an initially mono-energetic stellar tracer with rh0/rmx0 = 1/64, embedded deeply in the density cusp of a dark matter halo. The (dark matter) mass sourcing the underlying potential is reduced impulsively, in a single step, to values of ﹩{\mathrm{log}}_{10}M/{M}_{0}=-0.4﹩, −1.0, −2.0. The density profile develops a tail toward larger radii, which for M/M0 ≲ 1/100 is well approximated by a power law. The stellar tracer retains centrally isotropic kinematics, but is heavily radially biased in the outskirts. For the model with M/M0 = 1/100, a slight overdensity develops with tangentially biased kinematics, located close to the initial truncation radius rt0 (Equation (18)). Dotted curves show a model (Equation (B5)) for the outer density profile that assumes purely radial orbits for an energy distribution as in Figure 11 (see Section 4.3 and Appendix B for details). Right panels: the same as in the left panels, but for an extended stellar tracer with rh0/rmx0 = 1/4. At large radii, the log-slope of the stellar density profile approaches ﹩{d}\,{\mathrm{ln}}\,{\nu }_{\star }(r)/{d}\,{\mathrm{ln}}\,r\to -4﹩.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Like Figure 5 but showing the equilibrium half-light radii rh and average velocity dispersions ﹩{\langle {\sigma }^{2}\rangle }^{1/2}﹩ reached after an impulsive change to the underlying potential. All simulations start from the same initial conditions (⨂) that lie along the thick gray curve labeled M/M0 = 1. The mass sourcing the underlying potential is then lowered, in a single step, by 0.2 dex, 0.4 dex, … , 2 dex, and the system is allowed to return to an equilibrium state (○). The area of the individual points corresponds to the fraction of remnant (bound) stars N⋆/N⋆0. Half-light radii and velocity dispersions are measured considering bound (﹩{ \mathcal E }\lt 1﹩) stars only. For reference, the adiabatic evolution is shown as a dashed curve. In the impulsive regime, the expansion of deeply embedded stellar population is accompanied by a smaller reduction in the velocity dispersion than in the adiabatic case. The stellar populations rapidly lose stars as their half-light radii rh approach the radius of maximum circular velocity rmx of the underlying dark matter halo.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Panel array (a): time evolution of the stellar tracer with rh0/rmx = 1/64, deeply embedded in a cuspy halo. At t = 0, the stellar tracer is subject to an impulsive perturbation as in Figure 13. Top panel: (2D) surface density (color-coded), projected onto the {x, y}-plane. A black circle with radius R = rh indicates the (3D) half-light radius. Bottom panel: radial velocity vr and (3D) radius r. The number of particles per bin is color-coded. A cross indicates the location of the half-light radius rh and the median radial velocity 〈vr〉. The stellar tracer embedded in a cuspy halo phase mixes rapidly toward an equilibrium configuration. Panel array (b): like panel array (a) but for a stellar tracer deeply embedded in a cored dark matter halo. Phase mixing takes substantially longer than in the cuspy case. Panel array (c): like panel array (a) but for an extended stellar tracer with initial half-light radius rh0/rmx = 1/4, embedded in a cored dark matter halo. In contrast to panel array (b), here, phase mixing progresses rapidly, as most stars of the stellar tracer are located outside the density core and hence span a wide range of orbital periods. For videos supplementing this figure, see Appendix C.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Like Figure 6 (bottom panel), but showing the relative change in remnant (dark matter) mass Mh = M(<rh) (enclosed within the new equilibrium half-light radius rh reached after an impulsive change to the underlying potential) as a function of the relative change in half-light radius rh/rh0. In addition to the data shown in Figure 9, here we include simulations for even stronger perturbations, spanning 1 ≥ M/M0 ≥ 1/1000. The area of individual points indicates the remnant number of (bound) stars N⋆/N⋆0. In the linear regime, the final equilibrium states coincide with the adiabatic case. For the nonlinear regime, the mass enclosed within the stellar half-light radius increases as the half-light radius expands, until stars are lost.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Equilibrium configurations of half-light radius rh and average velocity dispersion ﹩{\langle {\sigma }^{2}\rangle }^{1/2}﹩ reached after an impulsive change to the underlying potential. The mass sourcing the potential is decreased to a value of M/M0 = 10−1.4 in n = 1, 2, 4, 8, and 16 discrete steps (shown in red, blue, green, purple, and orange, respectively). The smaller the relative change in potential between two subsequent steps (i.e., the more linear are perturbation and response), the closer the overall evolution is to the adiabatic case. As an example, for the cases of n = 1 and n = 2, the full time evolution toward the equilibrium states is depicted using dotted curves.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Like Figure 9, but showing the equilibrium half-light radius rh and velocity dispersion ﹩{\langle {\sigma }^{2}\rangle }^{1/2}﹩ reached after an impulsive deepening of the underlying potential. The (dark matter) mass sourcing the underlying potential is increased impulsively, in a single step, by +0.2 dex, +0.4 dex, … , +2 dex. In response to the impulsive increase in mass, the half-light radii contract, and the velocity dispersion increases. The same systematics are observed for stellar tracers embedded in a cored dark matter halo (not shown).