adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Fitting result of the radial profiles of X-ray surface brightness and photon index for forcing zero proton fraction. In this case, the parameters are as follows: η  B  = 0.9972, η  e  = 2.818 × 10−3, α = 1.91, β = 0.33 and ϵ = 0.52.
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The corner plot of the MCMC fitting for the convection-dominated scenario.
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The corner plot of the MCMC fitting for the convection–diffusion scenario.
Paper: Puffy Venuses: The Mass–Radius Impact of Carbon-rich Atmospheres on Lava Worlds
Authors: Bo Peng, 博 彭, Diana Valencia
Figure caption: Left: sample atmospheric profiles with different κ th and γ treatments, benchmarked to the Venusian atmosphere (A. Seiff et al. 1985) at different latitudes (thick gray lines)—dashed line: 45°; dotted line: 85°; dashed–dotted line: 0°–30°. Red-dashed line: κ th = C · P; red-dashed–dotted line: κ th = a · P + b. The low and high γ cases use γ's that are 1/5× and 5× of fiducial, respectively. Right: atmospheric height as a function of κ th and γ choices for an Earth-mass planet with fiducial T eq and bulk volatile abundance. The black-dashed line represents the excess radius an Earth-mass planet would produce if it had no iron (i.e., Fe/Si = 0).
Paper: Puffy Venuses: The Mass–Radius Impact of Carbon-rich Atmospheres on Lava Worlds
Authors: Bo Peng, 博 彭, Diana Valencia
Figure caption: Graphite activity at the MO surface, as a function of planet mass, T eq, and bulk volatile budget. Line colors correspond with different T eq = 1000, 1500, and 2000 K. Dashed line is the threshold of graphite saturation. Left: planets with C and H abundances of OC chondrites. Middle: those of CI chondrites. Right: those of ECs.
Paper: Puffy Venuses: The Mass–Radius Impact of Carbon-rich Atmospheres on Lava Worlds
Authors: Bo Peng, 博 彭, Diana Valencia
Figure caption:  M–R relations relative to 55 Cnc e. Lines with the same color share the same bulk C and H abundances. Dashed lines use 55 Cnc’s C/O = 0.78 (J. K. Teske et al. 2013); solid lines use the solar C/O = 0.55.
Paper: Broadband Spectral Modeling of the M87 Nucleus
Authors: Andrzej Niedźwiecki, Michał Szanecki, Agnieszka Janiuk
Figure caption: Comparison of the observed SED of the M87 core with spectra predicted by (a) the analytic ADAF model and (b, c) the model based on the GRMHD simulation. In all panels the green points show the highest-spatial-resolution SED in the quiescent phase of M87* given in Table 4 of M. A. Prieto et al. (2016), and the blue points show results of the quasisimultaneous multiwavelength campaign in 2017, reported by EHT MWL Science Working Group et al. (2021). See Table 1 for definition of the models. All models assume M = 6.5 × 109 M ⊙ and i = 17°; all spectra except for the dotted magenta line in (c) assume a purely thermal distribution of electron energy. In panel (a) the solid red line shows the spectrum of the kerrflow model A1; the dashed black line shows the spectrum of riaf-sed (R. S. Nemmen et al. 2014) for the same ﹩\dot{m}={10}^{-5}﹩, δ = 0.1, and β = 1. The difference between the model spectra is primarily due to the neglect of GR effects and the inaccurate treatment of Comptonization in riaf-sed. Panel (b) illustrates how the GR transfer affects the spectrum in the GRMHD model B; the synchrotron and Compton components are shown separately. The dashed black line shows the spectrum in the flat spacetime (i.e., neglecting the GR transfer) and the solid red line shows the fully GR spectrum. Panel (c) shows how the Compton component is affected when the synchrotron component is matched to the data by increasing either the magnetic field (the solid red line, model D) or the density and the electron temperature (the dashed black line, model C). The synchrotron and Compton components are shown separately. The dotted magenta line shows the synchrotron spectrum in model D with a hybrid electron energy distribution, including a 5% energy content of nonthermal electrons in the form of a high-energy power-law tail with an index equal to 3.2.
Paper: Broadband Spectral Modeling of the M87 Nucleus
Authors: Andrzej Niedźwiecki, Michał Szanecki, Agnieszka Janiuk
Figure caption: Comparison of the radial profiles of (a) T p, (b) B, (c) n, and (d) T e for the kerrflow models A1 (the dashed green lines) and A9 (the dotted blue lines) and the GRMHD model A (the red solid lines), see Table 1. In panel (d), the dotted–dashed black line is for the R–β relation, Equations (1) and (2), with R high = 80, R low = 1; the solid red line is for T e = 0.04T p assumed in most of our spectral models. In the GRMHD model, T p, B, and T e are found by spherical, density-weighted averaging (over narrow shells with Δr = 0.1r), and n by averaging over narrow rings (again with Δr = 0.1r) with z ≤ 0.1r.
Paper: Characterizing the Nanohertz Gravitational Wave Background Using a t-process Power Spectral Density
Authors: Shashwat C. Sardesai, Joseph Simon, Sarah J. Vigeland
Figure caption: The recovered log PSD (top) and the distribution of Hellinger distances (bottom) comparing all 50 of the holodeck simulations in blue to the pure power-law simulations (null hypothesis) in red for the 14th frequency component (27.7 nHz), where a major deviation from the power law occurs. The astrophysically realistic simulations have a 90% confidence interval between 0.022 and 0.457, whereas the null distribution has a 90% confidence interval between 0.027 and 0.104. The bottom panel shows the log-PSD posteriors (blue), and the black curve indicates the convolution of the ﹩\mathrm{log}{A}_{\mathrm{gw}}﹩, γ gw posteriors and the inverse gamma prior. At the this frequency component, the posterior tends to search over the entire prior space, but we see a deviation for some simulations, which are able to detect the presence of excess noise at 27.7 nHz. Simulations with HD < 0.1 are the closest to the prior, whereas simulations with HD > 0.1 display the bimodality of the posterior in the bottom panel.
Paper: Broadband Spectral Modeling of the M87 Nucleus
Authors: Andrzej Niedźwiecki, Michał Szanecki, Agnieszka Janiuk
Figure caption: The dashed red lines show the volume-filling factors of the regions with a given value of (a) the electron temperature and (b) the magnetic field in model A at r ≤ 4. The solid blue lines show a similar distribution of the regions with a given value of these parameters, but weighted by the synchrotron emissivity, which then gives the contribution of these regions to the total synchrotron emission. The dotted black line in panel (a) shows the distribution of T e weighted by the synchrotron emissivity for the R–β relation with R high = 80 and R low = 1.
Paper: Characterizing the Nanohertz Gravitational Wave Background Using a t-process Power Spectral Density
Authors: Shashwat C. Sardesai, Joseph Simon, Sarah J. Vigeland
Figure caption: Reconstructed GWB PSD for the holodeck simulations using a t-process model (blue), free spectral model (red), and power-law model (green). The violins and shaded region show the 90% confidence interval. The injected PSD is shown as the black dashed line. The t-process model is best able to recover the injected PSD, while the free spectral model and power-law model recover the injected PSD well at low frequencies but not at high frequencies.
Paper: Characterizing the Nanohertz Gravitational Wave Background Using a t-process Power Spectral Density
Authors: Shashwat C. Sardesai, Joseph Simon, Sarah J. Vigeland
Figure caption: Corner plots of all 50 holodeck simulations. The blue contours and histograms are for the t-process, while the green histograms and contours are for the standard power-law recovery. The green and blue dashed lines indicate the 1σ confidence interval. We see that both models recover the same log A and gamma values, but the t-process can also detect the presence of a deviation at 27.7 nHz, which was seen in Figure 7, whereas the t-process cannot detect such a deviation. We also see that α 14 component searches over more of the inverse gamma prior. The ﹩\mathrm{log}{\alpha }_{i}﹩ distributions not shown here peak between 0.13 and 0.3, with increasing variance as we go to higher frequencies.
Paper: Broadband Spectral Modeling of the M87 Nucleus
Authors: Andrzej Niedźwiecki, Michał Szanecki, Agnieszka Janiuk
Figure caption: The dots represent the contribution from a given radial bin (for logarithmic radial grid) to the flux observed at different frequencies at i = 17° in model D, normalized by the flux measured by VLBA at 4.3 × 1010 Hz, GMVA at 8.6 × 1010 Hz, EHT at 2.3 × 1011 Hz, and HST at 5.2 × 1014 Hz, as reported by EHT MWL Science Working Group et al. (2021).
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Afterglow light curves at 5.5 GHz for θ obs = 18° for several jet models with different opening angles, L j = 1050 erg s−1 (top) and L j = 1051 erg s−1 (bottom), which use the E Ω modeled after the fitting curves shown in Figure 11 (the same color scheme). In the upper panel, we report only three synthetic light curves out of four, since the model for θ j = 10° with L j = 1050 erg s−1 has unrealistic values for n 0 and ε B. The radio points and relative fit (black dashed line) are taken from E. Troja et al. (2019). The dashed lines are the afterglow from the generalized Gaussian fits only, while the solid lines are the light curves of the jet, including the energy distribution outside the Gaussian fits. For comparison, alongside the value of the jet opening angle, we report θ c from the fit.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Jet energy per solid angle for jets with constant luminosities of L j = 1050 erg s−1 (top panel) and 1051 erg s−1 (bottom panel). In each figure, we report the distributions for θ j = 3° (orange line), θ j = 5° (blue line), 6.8° (green line), 10° (red line), and 20° (purple), with an injection time of t e = 300 ms, and their respective generalized Gaussian fits (solid, dashed, dotted, dashed-dotted, and solid black lines). The dashed colored lines for each run indicate the energy per solid angle of the sole jet material. The fit parameters refer to Equation (6). The gray line represents the initial ejecta’s energy per solid angle. The minima in the calculated distribution are most likely due to the artificial axial symmetry that produces a “plug” ahead of the jet. The total energy for each jet model is 3 × 1050 erg.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Time evolution of the parameters of the generalized Gaussian fit for four jet simulations with θ j = [3, 5, 6.8, 10]° and L j = 1051 erg s−1. A specific color and marker identify each run in each plot. The top-left panel shows E 0 multiplied by an integration factor that depends upon θ c and the shape parameter normalized to the jet energy E j, namely ﹩f({\theta }_{{\rm{c}}},s)=2\pi {\theta }_{{\rm{c}}}^{2}[{c}_{1}(s)-{c}_{2}(s){\theta }_{{\rm{c}}}^{2}]﹩. The top-right panel shows the ratio θ c/θ j vs. time. Analogously, the bottom-left panel shows the shape parameter s vs. time, and the bottom-right parameter shows the linear correlation between θ c and the shape parameter.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Peak position, peak height, and peak spread of the afterglow curves as a function of the viewing angle θ obs, for four different opening angles: 3° (blue points), 5° (orange), 6.8° (green), and 10° (red). We superpose the points of the power-law fitting lines with the same color as the points. The viewing angle is normalized with respect to the jet opening angle of the corresponding run. In contrast, T peak and ﹩{{ \mathcal F }}_{\nu ,\mathrm{peak}}﹩, for simplicity, are normalized with respect to their values for θ obs = 60° (the last point of the series).
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Comparison between the formula used in H. van Eerten et al. (2010) for the shock proper velocity and our broken power law expressed by Equation (D4). The curves are plotted in dimensionless time t * and are scale-free. The dashed vertical lines indicate the two transition times t 1 and t 2 between the relativistic, transrelativistic, and the transrelativistic and Newtonian regimes, respectively. The horizontal dotted lines represent the values of u sh at the transition times. Our formula interpolates the two asymptotic regimes for t * → 0 and t * → ∞ with a softer power law between the two with u ∝ t −0.9.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Jet injection with initial conditions t d = 1 s for a jet with a wide initial opening angle of θ j = 35° and L j = 1051 erg s−1. The jet is shown at two different moments: top row—at t j = 25 ms; and bottom row—at t j = 150 ms. The solid white line is the initial opening angle at which the jet is injected, and the dashed line in the bottom row shows the actual—approximate—opening angle of the jet ≃10°. The external pressure could collimate the flow to a narrower angle in a few tens of milliseconds. Again, the four panels, from left to right, represent the Γβ factor, the density ρ, the pressure P, and the jet tracer (flagged cells with jet material advected with the fluid).
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Differential energy distribution with respect to the proper velocity Γβ of relativistic jets with L j = 1051 erg s−1 and θ j = [3, 5, 6.8, 10]° after 300 ms of injection. The solid lines represent runs with h j = 100 and Γj,0 = [12, 8, 6, 4], respectively, such that the final Lorentz factor Γ∞ = Γj,0 h j is not fixed. The dashed lines represent runs with the same opening angles but fixed Γ∞ = 500.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Comparison, after t j = 300 ms, between the velocity maps of two jets with the same opening angle θ j = 3° and L j = 1051 erg s−1, but different Γ∞. We have modified the color map and scale with respect to the other velocity maps to enhance the difference between the two runs. Notice the similarity in the overall structure.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Jet injection with initial conditions t d = 1 s for a jet with a wide initial opening angle of θ j = 20° and L j = 1051 erg s−1 (top row) and L j = 5.4 × 1051 erg s−1 (bottom row), at t j = 150 ms.
Paper: A Catalog of Pulsar X-Ray Filaments
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: Results of a search for filament candidates among CXO observations. The pink and purple background represent strong / weak acceptance regions for filament candidates; low Δ and high σ are preferred. Blue points represent known filaments or candidates listed in this work, brown represent known nonfilament PWNe, and the three orange points are filament candidates caught by the search. Radii scale logarithmically with total exposure time. For trails, a small circle shows the elevated significance arising from antialignment with the proper motion. Axes are shifted-logarithmic to better display data with σ or Δ near zero. An online version together with images of each pulsar is available at https://jack-dinsmore.github.io/filament-website/filament.html (Permanently hosted on Zenodo at: doi:10.5281/zenodo.13830862 (J. Dinsmore 2024)).
Paper: A Catalog of Pulsar X-Ray Filaments
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: Gate fractions g (Equation (9)) of all pulsars discussed in this work. The leftmost three are known filaments (a dotted circle marks the J2030 position with density enhancement), the next seven are newly observed nondetections, the rightmost two columns are archival survey pulsars with known proper motion, and the rightmost curve represents those with unknown proper motion as a probability distribution. Points have the same colors as in Figure 3, radius proportional to ﹩\mathrm{log}(\dot{E}/{d}^{2})﹩. The background indicates suggested gate fraction cuts. Error bars indicate combined velocity and n ISM uncertainties.
Paper: A Catalog of Pulsar X-Ray Filaments
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: The highest-g snapshot survey source produces the best signal from the automatic search; a trail (green) of 8.2σ significance when searched over the small proper motion range (103 yr length, white). Shown here is a CXO ACIS 1–7 keV adaptively smoothed image. The next-best feature found is at a large angle (cyan), and is not significant at just over 1σ. A substantially deeper observation would be required to map the trail and check the validity of this weak filament candidate.
Paper: A Catalog of Pulsar X-Ray Filaments
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: Filament spectra as observed by CXO with best-fit absorbed power laws. Though the data shown are background-subtracted, we perform the fit on unsubtracted data in order to preserve the signal-to-noise ratio.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Example products from RADMC3D radiative transfer simulations. Panel (a) is a channel map at V ch = 2.0 km s−1 directly produced from a FARGO3D simulation output. Panel (b) is a channel map produced from the same FARGO3D simulation but with density and all three velocities azimuthally averaged. Panel (a-b) is the difference between the two. Contours in panel (a-b) are at 3σ = 3 mJy beam−1 level (both positive and negative), and they are overplotted in panels (a) and (b). The planet’s orbit is indicated by the black dashed ellipse, and the arrow indicates the direction of Keplerian rotation. The planet’s location is indicated by the cyan marker, and its size is set to 0.4R H, the expected size of the circumplanetary disk. The disk near side and far side are annotated. We put the disk at a distance of 100 pc. The synthesized beam is depicted in the bottom right of each panel. The color bars are in linear scale.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Group (a) panels: the nonaxisymmetric components in V  r  at 2h at 100, 300, and 1000 orbits (left column) and their differences (right column). Group (b) and (c) panels: similar to group (a) panels, but for V  ϕ  (b) and V  θ  (c). The location of the planet is indicated by the cyan marker, and its size is set to 0.4R H, the expected size of the circumplanetary disk. The trajectories of the spirals in the surface density are indicated by the small green circles (also shown in Figure 1). Gap edges at r = r p − 2R H and r p + 2R H are marked with gray dashed circles. The magenta ellipse indicates the gas structure at L5. The two ends of the horseshoe flow inside the gap are indicated by black arrows, and the strong converging flows are indicated by cyan arrows. The color bars are in linear scale. See Section 3.1.2 for details.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Convergence tests with simulations at four numerical resolutions: cells per scale height (CPH) around the planet of 7, 10, 14, and 20. The top row shows the differences between two runs with CPH = 7 and 10 in nonaxisymmetric velocity perturbations at 2h away from the midplane at 1000 orbits for the three velocities. The middle and bottom rows show the differences between the simulations with CPH = 10 and 14 and the simulations with CPH = 14 and 20, respectively. The primary inner and outer spiral density waves are marked by open green circles. Gray dashed lines indicate the inner and outer gap edges. The location of the planet is indicated by the cyan marker, and its size is set to 0.4R H, the expected size of the circumplanetary disk. The color bar is in a linear scale. See Section 3.2 for discussions.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Residual channel maps (the same kind as panel (a-b) in Figure 8) of the simulation with CPH = 20 at V ch = 0.6 (the (a) panels), 1.6 (b), and 2.2 km s−1 (c). Results at 100, 300, and 1000 orbits are shown from top to bottom. Planet-induced nonaxisymmetric kinematic signatures evolve with time. The planet is positioned at the position angle ϕ p = 315° in the disk frame. Residual emissions stronger than 3σ = ± 3.0 mJy beam−1 are marked with green contours. In each panel, the blue dashed curve represents the primary spirals at 2h away from the midplane, and gray lines mark the inner and outer gap edge. The beam size is displayed at the bottom left. The disk rotation direction is marked in panel (a1). The color bar is in a linear scale. See Section 4.2 for discussions.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Successive residual channel maps of the same kind as panel (a-b) in Figure 8 of the simulation with CPH = 20 at 1000 orbits. Signals in the maps highlight nonaxisymmetric velocity perturbations induced by the planet. Potentially detectable residuals are highlighted by 3σ contours (green). We only mark 3σ signals with a size bigger than the beam. Such signals are most prominently present in channels at V ch = 1.8–2.2 km s−1 (highlighted with a red frame). Gray and blue dashed lines denote gap edges and the primary spirals, respectively. The location of the planet is indicated by the cyan marker. The disk rotation direction is marked in the lower left panel. The color bar is in a linear scale. See Section 4.1 for further discussions.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: The three components in nonaxisymmetric velocity perturbations along the primary spiral density waves (traced out by the green circles in Figures 1 and 6) at 2h away from the midplane at 1000 orbits for four simulations with different numerical resolutions: cells per scale height (CPH) of 7, 10, 14, and 20. We exclude the region within R H from the planet at 100 au due to insufficient resolution in the circumplanetary region. The velocity field along the spirals is converging with resolution. See Section 3.2 for further discussions.