adsabs/AstroCLIMB huggingface dataset:
Paper: Electron Acceleration at Quasi-parallel Nonrelativistic Shocks: A 1D Kinetic Survey
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Snapshot of proton and electron x–p  x  phase spaces at ﹩t=225\,{\omega }_{\mathrm{ci}}^{-1}﹩ for v pt/c = 0.05, 0.1, and 0.2 (top to bottom), where other parameters, ﹩{{ \mathcal M }}_{{\rm{A}}}=20,{{ \mathcal M }}_{{\rm{s}}}=40,﹩ and m R = 100, are fixed. While the proton phase spaces (left panels) are quite similar for different v pt, there are fewer upstream electrons (right panels) for larger shock speeds.
Paper: Hybrid Simulations of the Martian Magnetotail Twist
Authors: Jingyi Zhou, Kaijun Liu, Riku Jarvinen, Esa Kallio, Kun Cheng, Shuai Zhang, Qi Liu, Yuqi Liu, Yan Wang, Ruohan Wang, Xinye Wang, Xuanyu Shang, Zhongyuan Xu, Yi Yuan
Figure caption: Maps of the X-component of the SW ion flow velocity (V  X,SW) in the XY plane at three different Z-values (as labeled) in Runs B1 (top) and D1 (bottom). In each panel, the horizontal black dashed line indicates Y = Y NS, while the white circle represents the projection of Mars.
Paper: Electron Acceleration at Quasi-parallel Nonrelativistic Shocks: A 1D Kinetic Survey
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Time evolution of downstream proton (dashed–dotted lines) and electron (solid lines) spectra for v pt/c = 0.05, 0.1, and 0.2, The designations of different panels are kept identical to Figure 3. The gray curves show the fitted thermal Maxwellian. Both protons and electrons show the NT tail. Panel (c) shows that the electron NT tail stalled.
Paper: Hybrid Simulations of the Martian Magnetotail Twist
Authors: Jingyi Zhou, Kaijun Liu, Riku Jarvinen, Esa Kallio, Kun Cheng, Shuai Zhang, Qi Liu, Yuqi Liu, Yan Wang, Ruohan Wang, Xinye Wang, Xuanyu Shang, Zhongyuan Xu, Yi Yuan
Figure caption:  XZ cuts of the X-component of the planetary ion momentum density in Run B1 at different Y-values as labeled. The white circle represents Mars in each panel.
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: Representative illustration of all of the candidate DM profiles (gray) we probed for each of the dEs in the sample. The color-coding for each dE we use in this study is indicated in the bottom-right panel. The candidate models are obtained by sampling the Zhao-like mass description (Equation (2)) on the parameter grid discussed in Section 3.2. In detail, the exact values of the sampling steps differed slightly from galaxy to galaxy, which is not shown here. To show the diversity in allowed profiles, we separated the candidate models into the different panels shown here according to their respective γ in and γ out. For simplicity, we only plotted the spherical models (q DM = 1.0). For comparison, we also overlay the stellar density distribution that we found for each of the dEs in our sample (colored lines).
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: The ΔAICp envelopes of the orbit models probed for each dE. The upper three panels, which are concerned with the luminous model components, were discussed in VW–I. The gray shaded panels show the parameters that describe the “dark” components of the orbits models, i.e., the black hole and DM. As argued in Section 3.2, the parameters that generate the halo distribution should be treated as nuisance parameters; specifically, γ in, γ out, and r s are very intercorrelated when the FOV is limited (as is always the case).
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: Table with Some of the Important Quantities We Measured. From left to right: the average DM density within 1r e in solar masses per cubic kiloparsec; the mass-weighted slope (Equation (6)) of the total density; the volume-averaged slope η DM within 0.8 kpc (Equation (4)); the axis ratio of the halo; the (mean) axis ratio of stars; the DM fraction within 1r e; the single stellar population (SSP) age in gigayears; metallicity; [Mg/Fe] ratio at r = 2.″5; stellar angular momentum in [kpc km s–1]; and the angular momentum parameter. Total stellar mass and distance to M87 are tabulated in VW–I.
Paper: The Binary Black Hole Merger Rate Deviates from the Cosmic Star Formation Rate: A Tug of War between Metallicity and Delay Times
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: The formation yield of BBHs, BHNSs, and BNSs that will merge within a Hubble time, per solar mass of star formation, ﹩{d}{{ \mathcal R }}_{\mathrm{form}}/{d}{M}_{\mathrm{SFRD}}﹩, as a function of birth metallicity, Z  i , for all models. We choose initial metallicities for each binary by sampling randomly from a log-uniform metallicity distribution from Z  i  = 0.0001 to Z  i  = 0.03. We then obtain ﹩{{ \mathcal R }}_{\mathrm{form}}({Z}_{i})﹩ using a kernel density estimation over the initial metallicities of the simulated binaries. The decline in BBH formation efficiency at Z  i  ≳ Z ⊙/5 is clearly visible.
Paper: The Binary Black Hole Merger Rate Deviates from the Cosmic Star Formation Rate: A Tug of War between Metallicity and Delay Times
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: Left: the BBH merger rate as a function of redshift for the α CE and β model variations explored in this paper compared to the SFRD scaled arbitrarily (black line). Right: the BBH merger rate divided by the SFRD, where we normalize the areas of both to one. The horizontal gray line indicates a merger rate that follows the SFRD, and the dashed vertical gray line is the redshift of the SFRD peak. In both panels we include the 1σ and 2σ confidence intervals calculated by bootstrapping the simulation results to show the sampling uncertainty (note that the uncertainties are typically the same size as the width of the lines). The sharp decline in the merger rate at z ∼ 9 is due to star formation starting at z = 10 in our calculations and the fact that mergers are delayed.
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: The shape of the N-body simulation’s density distribution approximated by an ellipsoid. Top: p = b/a, Bottom: q = c/a where a is the semimajor axis, b is the semi-intermediate axis, and c is the semiminor axis of the triaxial ellipsoid. The orange dots indicate the triaxial axis ratios of the stellar particle distribution. The orange line shows the corresponding axisymmetric approximation, which is also the edge-on “pseudo”-deprojection that we used for the dynamical modeling (but scaled by a variable mass-to-light ratio of the stellar population). The blue diamonds show the triaxial ratios of the DM particle distribution; it follows the shape of the stellar particles very closely, even outside the scouring core. The blue line shows the spatially constant DM flattening q DM of the best axisymmetric (oblate) orbit model we found. We sampled the axisymmetric flattening within  q DM ∈ [0.7, 0.8, 0.9, 1.0]. Similar to Figure 17, we mark regions smaller than the central spatial resolution and outside the FOV in red.
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: The minimum subtracted AICp constraints for the axisymmetric orbit models of the N-body simulation. In total, we calculated of the order of ∼5 × 103 orbit models. The red dots indicate the parameters of the best few models (ranked in AICp). The vertical dashed lines indicate the true stellar mass-to-light ratio and black hole mass.
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: Mass and anisotropy structure (spherically averaged) of the simulation (dots) and the recovered profiles of the best axisymmetric orbit model we were able to find (solid line). The dashed lines show the next best models when ranking all sampled models by their AICp; their nuisance parameters are indicated by the red dots in Figure 16. The inner red region indicates the typical size of our resolution limit. The outer red region marks areas outside the FOV. Panel (a): the total enclosed mass within radius r; panel (b): the local DM density; panel (c): the (cumulated) DM fraction (including the black hole); and panel (d): the anisotropy β of the stars.
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: Left: the mock observations for the triaxial N-body simulation. Right: the corresponding best axisymmetric model we found using our orbit modeling setup. Both mock and model LOSVDs are characterized here by a Gauss–Hermite series truncated at h 4. Higher-order deviations in the actual binned LOSVDs (that are still being modeled dynamically) are not shown.
Paper: The Binary Black Hole Merger Rate Deviates from the Cosmic Star Formation Rate: A Tug of War between Metallicity and Delay Times
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: Same as Figure 1, but for the BBH formation rate (formation is defined as the moment when the second BH forms). The peak of the BBH formation rate is clearly shifted to higher redshifts than the SFRD due to a higher BBH formation efficiency at lower metallicities.
Paper: The VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Christian Partmann
Figure caption: The same as for Figure 12 but for the central DM density ρ 0 (i.e., the maximum of the DM density). For the dEs, ρ 0 is measured as the average density within the central 100 pc, for the massive ETGs (J. Thomas et al. 2009) within 1 kpc. The dSphs and Sc-Im galaxies remain unchanged relative to Figure 12, because in both Figures we show the parameter ρ 0 = ρ(r = 0) of the cored halo profiles that these studies employ to model the halos.
Paper: Propagation of Gamma-Ray Burst Relativistic Jets in Active Galactic Nucleus Disks and Its Implication for Gamma-Ray Burst Detection
Authors: Hao-Hui Zhang, 浩辉 张, Jin-Ping Zhu, 锦平 朱, Yun-Wei Yu, 云伟 俞
Figure caption: Midplane density ρ 0 (left panel), disk scale height H (middle panel), and opacity κ (right panel) of AGN disks as a function of the radial distance r to the SMBH. The solid and dashed lines correspond to the SG and TQM disk models, respectively.
Paper: Propagation of Gamma-Ray Burst Relativistic Jets in Active Galactic Nucleus Disks and Its Implication for Gamma-Ray Burst Detection
Authors: Hao-Hui Zhang, 浩辉 张, Jin-Ping Zhu, 锦平 朱, Yun-Wei Yu, 云伟 俞
Figure caption: Velocity evolution of the jet head and jet remnant with the increasing height (top panels), as well as the corresponding observer timescale of the evolution (bottom panels). The SG disk model is adopted with different SMBH masses and GRB positions as labeled in the legend. The left, middle, and right panels correspond to different sets of luminosity and duration of the GRB jets. The locations of jet chokes are represented by solid points, while the crosses mark the locations of SBOs. The shaded area represents the typical location of internal shocks for normal GRBs.
Paper: Propagation of Gamma-Ray Burst Relativistic Jets in Active Galactic Nucleus Disks and Its Implication for Gamma-Ray Burst Detection
Authors: Hao-Hui Zhang, 浩辉 张, Jin-Ping Zhu, 锦平 朱, Yun-Wei Yu, 云伟 俞
Figure caption: Evolution of the opening angles of the jet head θ h and jet remnant θ jr (solid lines), as well as the jet cocoon θ c (dashed lines), as functions of the motion distance. The luminosity and duration of the GRB jet are fixed as labeled. Two disk models including the SG model (left panel) and TQM model (right panel) are considered, where the mass of the SMBH and the distance of the GRB position to the SMBH are labeled in the legend. The locations of jet chokes are represented by solid points.
Paper: Propagation of Gamma-Ray Burst Relativistic Jets in Active Galactic Nucleus Disks and Its Implication for Gamma-Ray Burst Detection
Authors: Hao-Hui Zhang, 浩辉 张, Jin-Ping Zhu, 锦平 朱, Yun-Wei Yu, 云伟 俞
Figure caption: Similar to Figure 3, but for the TQM disk model.
Paper: Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: J. Speicher, D. R. Ballantyne, P. C. Fragile
Figure caption: Left panel: the evolution of the normalization factor f  a , overplotted with the burst lightcurve (Equation (1), same as in Figure 1) for the a * = 0 (circle markers) and a * = 0.2 (cross markers) burst simulations. The size of the points in both panels increases with time. Their colors correspond to the shadings in Figure 1 for their respective time interval. With some scatter, f  a  follows the burst lightcurve for both simulations. Right panel: same as the left panel but shows the evolution of the mass accretion rate enhancement. Due to PR drag during the burst, ﹩{\dot{M}}_{\mathrm{enh}}﹩ calculated at r isco (Equation (5)) increases in the a * = 0 burst simulation (circle markers) from ≈1.6 to ≈9 and decreases again to ≈1.6. For the a * = 0.2 burst simulation (cross markers), ﹩{\dot{M}}_{\mathrm{enh}}﹩ is ≈10.6 in interval F and decreases to ≈3.7 in interval I.
Paper: Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: J. Speicher, D. R. Ballantyne, P. C. Fragile
Figure caption: Luminosity profile (Equation (1)) of the burst in the simulations by J. Speicher et al. (2023). The luminosity (black solid line) peaks at 1038 erg s−1 at ≈2.2 s. The shaded regions mark ≈0.4 s long time intervals, during which we time average the simulation data to calculate the disk emission (Equation (2)). Due to a transient numerical event, we only analyze the time intervals past the red dashed line for the a * = 0.2 burst simulation. For all no-burst simulations we use time interval F to calculate disk properties.
Paper: Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: J. Speicher, D. R. Ballantyne, P. C. Fragile
Figure caption: Left panel: plot of f  a  vs. ﹩{\dot{M}}_{\mathrm{enh}}﹩ for the a * = 0 simulation. The colors are the same as in Figure 1, and the marker sizes increase with time. f  a  and ﹩{\dot{M}}_{\mathrm{enh}}﹩ are weakly linearly correlated, with a Pearson coefficient of 0.63. Right panel: same as the left panel, but for the a * = 0.2 simulation. Here, scatter affects the f  a  vs. ﹩{\dot{M}}_{\mathrm{enh}}﹩ relationship more significantly than for the a * = 0 simulation. The correlation between ﹩{\dot{M}}_{\mathrm{enh}}﹩ and f  a  is only positive when restricting the time intervals E–I, with a correlation factor of 0.56.
Paper: Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: J. Speicher, D. R. Ballantyne, P. C. Fragile
Figure caption: Left panel: radially integrated disk spectra of the a * = 0 simulations. The spectra are integrated between the respective inner disk radius and 300 km (Equation (2)). The time intervals and line styles are the same as in Figure 2. Right panel: same as the left panel, but for the a * = 0.2 simulations, and the spectra of time interval D instead of A are shown.
Paper: Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: J. Speicher, D. R. Ballantyne, P. C. Fragile
Figure caption: Radial temperature profile of the a * = 0 burst simulations for intervals A (blue solid line), E (red dotted line), and F (green dashed–dotted line). The temperature profile of the no-burst simulation (black dashed line) is from interval F. The temperatures are located where the optical depth due to Thomson scattering, integrated toward the equatorial plane, first surpasses 1 and is equated to T eff for Equations (2) and (3). The plotted temperature profiles have been smoothed for visualization by calculating moving averages with varying window sizes.
Paper: Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: J. Speicher, D. R. Ballantyne, P. C. Fragile
Figure caption: Left panel: Pearson correlation coefficient between ﹩{f}_{\tilde{a}}﹩ (Equation (6)) and ﹩{\dot{M}}_{\mathrm{enh}}﹩ (Equation (5)) as a function of energy. For both the a * = 0 (solid line) and a * = 0.2 (dashed line) simulations, ﹩{f}_{\tilde{a}}﹩ correlates most strongly with ﹩{\dot{M}}_{\mathrm{enh}}﹩ at energies below 1 keV. Right panel: the range of ﹩{f}_{\tilde{a}}﹩ for the a * = 0 (solid line) and the a * = 0.2 (dashed line) simulations. With decreasing energy below ≈10 keV, and with increasing energy above ≈10 keV, ﹩{f}_{\tilde{a}}﹩ varies less.
Paper: Propagation of Gamma-Ray Burst Relativistic Jets in Active Galactic Nucleus Disks and Its Implication for Gamma-Ray Burst Detection
Authors: Hao-Hui Zhang, 浩辉 张, Jin-Ping Zhu, 锦平 朱, Yun-Wei Yu, 云伟 俞
Figure caption: Parameter space in the (r, M SMBH) plane for jet choking (gray region) and breakout (blue region). The top and bottom panels correspond to the SG and TQM disk models, respectively. The adopted jet duration and luminosity are labeled in the legend.
Paper: Propagation of Gamma-Ray Burst Relativistic Jets in Active Galactic Nucleus Disks and Its Implication for Gamma-Ray Burst Detection
Authors: Hao-Hui Zhang, 浩辉 张, Jin-Ping Zhu, 锦平 朱, Yun-Wei Yu, 云伟 俞
Figure caption: An illustration of the different results of jet propagation in AGN disks.
Paper: Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: J. Speicher, D. R. Ballantyne, P. C. Fragile
Figure caption: Top row: the disk spectra (red dotted lines, same as in Figure 3) do not surpass the burst spectra (black solid lines) in time interval E for either the a * = 0 (left column) or a * = 0.2 (right column) simulation and thus do not contribute to a soft excess. Bottom row: same as the top row, but instead of true disk spectra, no-burst spectra multiplied by f  a  are plotted. The scaled no-burst spectra exceed the burst spectra at low energies and generate an apparent soft excess. The shift of disk spectra to higher energies (top row) versus their unchanged shape (bottom row) reduces their contribution to the soft excess.
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: The gray-scale image shows the PLCK171 core region, observed with the HST/ACS filter (A. Acebron et al. 2018). The blue contours are from the high-resolution image at 610 MHz (IMG3) and drawn at [3, 9, 27, 81]×σ rms, where σ rms = 37 μJy beam−1 is the noise level, with a beam size of the image is 5.″5 × 4.″5. The different colored circle indicates the detection of the optical counterpart of each radio source. Their naming conventions (S7 is out of the HST image) are annotated in the image, and similar to S. Giacintucci et al. (2013).
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: Left:  The cluster central diffuse sources are shown in a low-resolution (21″) image (IMG2) at 400 MHz. The contour (gray) levels are drawn at [1, 2, 4, 8...]× 3σ rms, where σ rms = 50 μJybeam−1 is the noise level. The overlaid red contour is from the JVLA D-array image (IMG5), drawn at a significance of [1, 2]×  3σ rms, with σ rms = 29 μJy beam−1, with a beam size of 35″ ×  35″. The blue-lined sector marks the AGN, which is seen to be connected with the radio halo. Right:  Here we show the 21″ JVLA C- and D-array combined image (IMG4) of the cluster field at 1400 MHz. The gray contours are drawn at a similar significance level, with a σ rms = 23 μJy beam−1. The red contours are drawn from JVLA D-array images, just for a comparison of the extension of the diffuse emission.
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: Left: point-source-subtracted image of the cluster central field for 400 MHz at 25″×25″ (black circle at bottom left corner) is shown. The green circle indicates the detection of source “U” at significance >3σ rms. Contour levels are drawn at [1,2,4,8...]×3σ rms, where σ rms = 60 μJy beam−1. Right: point-source-subtracted image at 1400 MHz, with a similar beam size. The rms noise of the image is 30 μJy beam−1 and the spacing of the contour level is similar to the left image.
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: Radio vs. X-ray surface brightness (on a logarithmic scale) plots for the halo in PLCK171 at 400 and 1400 MHz are shown. The LinMix best-fit line is shown in the solid (red & black) lines. The red and black circles show the detection of the radio halo above 3σ rms. The 2σ rms are considered as the upper limits and indicated by arrows (cyan for 400 and orange for 1400 MHz). The red and black dashed line shows the 1σ rms line for different frequencies. The inset image shows the diffuse X-ray emission in gray color, and radio emission in blue contours. The magenta grids are (25″) the regions used for estimating the radio and X-ray surface brightness.
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: Integrated radio spectral index for the radio halo between 235 and 1400 MHz. The black dashed line shows the overall spectrum of the halo following a single power law from our analysis. The black points denote the flux density values at each frequency in our work. The power law fit from the S. Giacintucci et al. (2013) is shown for their 235 and 1400 MHz measurements in red points. The annotated figure shows the 400 MHz radio halo emission (in color), and the green circle shows the radio halo region, which is used to estimate the flux density.
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: Left: The spectral index map for the radio halo in PLCK171 at 25″ is shown between 400 and 1400 MHz. The black contours are drawn at 3σ rms×[1, 2, 4, 8..] from the 400 MHz image. Right: The corresponding error map is shown here. The procedures for the estimation of the error map are followed as described in F. de Gasperin et al. (2017).