adsabs/AstroCLIMB huggingface dataset:
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Predictions of the dual AGN fraction as a function of redshift from our sample in ROMULUS (blue solid line) compared to other cosmological simulations: ASTRID (N. Chen et al. 2023), HORIZON-AGN (M. Volonteri et al. 2022), EAGLE (Y. M. Rosas-Guevara et al. 2019) with green, red, and purple lines respectively. The error bars show 1σ standard deviation. We also show the dual fraction in ROMULUS with a separation criterion of 4 kpc < Δr < 30 kpc with a dashed blue line. Observational estimates and predictions are presented with gray square (predictions for upcoming AXIS surveys, A. Foord et al. 2023), gray triangle (M. Koss et al. 2012), and gray circle (X. Liu et al. 2011).
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Comparative distribution of AGN Host Properties. The left panel displays the stellar mass distribution, the center panel shows the specific star formation rate gas mass distribution, and the right panel illustrates the gas mass distribution for single (gray) and dual (cyan) AGNs inside a 30 kpc sphere around their host halo center.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: The total luminosity of two SMBHs in a dual AGN system vs. their combined mass. SMBHs within a dual system that eventually merge are represented with circles, while those that do not merge by z = 0 are represented by stars. In the top panel, the data points are color-coded based on the separation between the two SMBHs when they are detected as a dual AGN. The data points in the bottom panel are color-coded according to the time elapsed between the detection of the dual AGN and the merger of the two SMBH. The stars are shown in gray because the merging time is not applicable to them.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Evolution of dual AGNs that merge. The figure shows the evolutionary properties of a dual AGN system from the time that they were in two distinct halos until they merged (shown by a green star). We trace their masses (first panel), luminosity (second panel), surrounding gas density (third panel), and pair separation (fourth panel). The dashed vertical line shows the redshift that duals have been detected. We remind the reader that, in our study, detection is confined to selected epochs at z ≤ 2 (see Section 2.3). The dashed horizontal line is the luminosity threshold for AGN definition in our study.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Relationship between black hole mass and halo mass for dual AGNs. This scatter plot illustrates the primary AGN masses in orange and the secondary AGN masses in blue, plotted against their host halo mass. The dashed red line indicates the median trend of single AGNs for comparison. The shaded region encloses the scatter of the 16%–84% of the MBH in the halo mass bin. The histogram at the top displays the normalized count of the halo mass distribution for single AGN hosts in gray and for dual AGN host halos in cyan. Dashed lines show medians.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Distribution of separations between SMBHs in dual AGNs at redshifts under consideration. Each redshift is represented by a distinct color, with filled histograms indicating the count of dual AGNs at that specific redshift. The solid blue line outlines the combined count for all redshifts, illustrating the 3D physical separation between dual AGNs, while the dashed blue line represents the projected 2D separations on the x–y plane. The plot highlight a higher frequency of dual AGNs with separations less than 10 kpc, peaking around 2 kpc.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Scatter plot illustrating the ratio of bolometric luminosities to the mass ratio of primary to secondary supermassive black holes (SMBHs) in dual AGN systems. Each point represents a dual AGN, plotted with respect to the mass ratio on the x-axis and luminosity ratio on the y-axis. The dashed vertical line at M  p /M  s  = 1 demarcates equal mass pairs.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Count of AGN systems at different redshifts in the Romulus25 simulation, categorized by dual (orange), triple (green), and quadruple (red) AGNs. The number of single AGNs for each redshift is displayed in the table cells located below the corresponding bars in the chart.
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: The key results of this study. The top two plots are only for the accreting planets. The bottom plot includes results for nonaccreting planets as well. Magenta squares indicate measurements from the iterated simulations (see Section 2.4) and cyan squares indicate measurements from before iteration. Top: the planetary accretion rates ﹩{\dot{m}}_{{\rm{p}}}﹩. Middle: the torques on the planets ﹩{\dot{J}}_{{\rm{p}}}﹩. The magenta and cyan squares are total AM exchange, ﹩{\dot{J}}_{{\rm{p}}}={\dot{J}}_{{\rm{p}},{\rm{p}}}+{\dot{J}}_{{\rm{p}},{\rm{g}}}+{\dot{J}}_{{\rm{p}},{\rm{a}}}﹩, and the yellow, black, and green squares the components. Bottom: the orbital expansion/contraction rate, ﹩{\dot{a}}_{{\rm{p}}}﹩.
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: Same as Figure 6, but for Run II.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Gini feature importance provided by the random forest classifier for quenched regions defined in three different ways (panels from left to right): by D  n (4000) and EW(Hα) in this work, by BPT diagrams and EW(Hα) following L. Lin et al. (2019a), and by BPT diagrams and D  n (4000) following A. F. L. Bluck et al. (2020b, 2020a). In the upper panels, the same set of properties as used in Figure 6 are included in the analysis here. For the lower panels, a subset of properties similar to those used in A. F. L. Bluck et al. (2020b, 2020a) are included in the analysis. The properties are ordered by decreasing the feature importance resulting from the samples in the leftmost panel. The orange empty histograms in the rightmost panels show the results when the criterion of D  n (4000) >1.6 is adopted instead of D  n (4000) >1.45.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Each panel is an N2Hα vs. x-axis diagram. The x-axes are O3N2, Z *, and ﹩\mathrm{log}{t}_{\mathrm{age}}﹩ from left to right. The meanings of black contours and dots are the same as in Figure 1. The mean value and 1σ scatter of GRQRs and GPQRs are shown as red and green circles with an error bar, separately. In the left and center panels, the colorful contours show the distribution of ﹩\mathrm{log}﹩ stellar age. In the right panel, the colorful contours represent the ﹩\mathrm{log}{{\rm{\Sigma }}}_{* }﹩ distribution.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The distribution of resolved regions of our sample on the diagram of ﹩\mathrm{log}﹩EW(Hα) vs. D  n (4000) (left), ﹩\mathrm{log}﹩EW(Hα) vs. EW(Hδ  A ) (center), and ﹩\mathrm{log}﹩Σgas vs. D  n (4000)-﹩\mathrm{log}﹩ EW(Hα) (right). The red dots in each panel represent the sub-sample of “quenched regions,” which are defined jointly by BPT diagrams and EW(Hα)<3 Å following L. Lin et al. 2019a (upper panels), or jointly by BPT diagrams and D  n (4000)>1.45 following A. F. L. Bluck et al. (2020a, 2020b; lower panels).
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: No bias of the molecular gas estimator on parameters used in analysis. Different panels show the probability density distribution of residual (﹩\mathrm{log}{{\rm{\Sigma }}}_{{\rm{H}}{2}_{\mathrm{pre}}}-\mathrm{log}{{\rm{\Sigma }}}_{{\rm{H}}{2}_{\mathrm{CO}}}﹩) in different bins (represented by different colors) of different parameters. The parameters shown in the first row are E(B−V), Q  κ , and Σ*. The parameters in the second row are EW(Hα), D  n (4000), and N2Hα. The parameters in the third row are radius, galaxy mass, and corrected Hα flux. The vertical line in each panel is located at zero residual as a reference. The error bar shows 1σ uncertainty. The σ r,* used to calculate Q  κ  is approximated by line-of-sight σ * in this figure. All the test data used here are obtained from the EDGE-CALIFA sample.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Left and center panels, the comparisons of estimates of κ (left panel) and A (center panel) with the values given by the relations in Equations (4) and (5). For the x-axes of these two panels, we use Σb = Σgas + Σ* instead of Σm. The right panel illustrates the correlation between the Q value measured by κ and A. The 1:1 relationship is indicated by the blue line in each panel.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The upper panels (from left to right) display the radial profile of ﹩\mathrm{log}{Q}_{A}﹩, ﹩\mathrm{log}\tau ﹩, and ﹩\mathrm{log}{Q}_{A}\tau ﹩, with the distribution of ﹩\mathrm{log}{{\rm{\Sigma }}}_{* }﹩ indicated by the colorful contours in each panel. The lower panels show the correlation of ﹩\mathrm{log}{Q}_{A}﹩, ﹩\mathrm{log}\tau ﹩, and ﹩\mathrm{log}{Q}_{A}\tau ﹩ with ﹩\mathrm{log}{{\rm{\Sigma }}}_{* }﹩, with the distribution of R/R  e  shown as colorful contours in each panel. The black arrows indicate the systematic shift of ﹩\mathrm{log}\tau ﹩ and ﹩\mathrm{log}{Q}_{A}\tau ﹩ when the N2O2 method instead of the O3N2 method is utilized to estimate Z gas.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The F(ϵ Edd > 1), the fraction of spaxels with ϵ Edd > 1, as a function of Ψ for the parent sample as well as the two types of quenched regions. The solid lines show the results obtained by assuming a fixed value of k abs = 1, while the dashed lines show the results based on the estimates of k abs as derived from E(B − V).
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The examples of rotation curve fitting. Different columns represent randomly selected galaxies from our starting sample. The first row showcases the model ﹩v(R)={v}_{\mathrm{flat}}\,\left[1-{e}^{-R/{l}_{\mathrm{flat}}}\right]﹩, while the second row presents the model ﹩v(R)={v}_{\mathrm{flat}}\tanh \,\left(R/{h}_{\mathrm{rot}}\right)﹩. The black points in each panel denote every valid spaxel in the galaxy, with the blue curve representing the best-fitting result.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Consistency of κ and A obtained by rotation curve fitting and local gradient. The meanings of contours and black dots are the same as in Figure 1. The blue diagonal line in each panel shows a 1:1 correlation.
Paper: Self-similar Solutions of Oscillatory Reconnection: Parameter Study of Magnetic Field Strength and Background Temperature
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Evolution of the plasma flow for case D2, where B 0 = 10 G and T 0 = 1 MK. Panel (a) shows the contour of v ⊥ and separatrices, panels (b) to (d) present contours of ΔT = T − T 0, and black lines represent the (evolving) separatrices.
Paper: Self-similar Solutions of Oscillatory Reconnection: Parameter Study of Magnetic Field Strength and Background Temperature
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: (a) Maximum integrated temperature ﹩\langle {\rm{\Delta }}T{\rangle }_{\max }﹩ as a function of equilibrium magnetic field strength B 0. The brown dotted–dashed line denotes a fitted quadratic dependence on the magnetic field strength following ﹩\langle {\rm{\Delta }}T{\rangle }_{\max }\sim {B}_{0}^{2}﹩, where the slope is offset artificially for ease of comparison. (b) Maximum integrated nondimensional temperature ﹩\langle {\rm{\Delta }}T{\rangle }_{\max }﹩ as a function of internal-to-magnetic energy ratio. The purple line represents the maximum obtained for simulation set A seen in Figure 3. The red line represents the maximum from simulations B2, C2, and D2; the green line corresponds to simulations B3, C3, and D3; the orange line cases B4, C4, and D4; and the blue line cases B5, C5, and D5.
Paper: Self-similar Solutions of Oscillatory Reconnection: Parameter Study of Magnetic Field Strength and Background Temperature
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Left column displays variations of the current density at the null point, j  z (0, 0, t)/j 0, displays for different equilibrium magnetic field strengths, and initial background temperature configurations. Right column shows the PSD of j  z (0, 0, t)/j 0 of the same simulations.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Consistency of total gas mass surface density in our sample by using different H I estimators. The three panels from left to right show the pairwise comparison of the following three estimators: the fixed value at 6 × 106  M ⊙ kpc−2 (Σgas,6e6), J. Wang et al. 2016's model (Σgas,model) and stellar mass surface density–H I mass surface density relationship found by L. Morselli et al. (2020; Σgas,*). The blue dots in three panels are spaxels on which we use different H I estimators to obtain their total gas mass surface density. The diagonal red dashed lines in these panels show a 1:1 correlation.
Paper: Self-similar Solutions of Oscillatory Reconnection: Parameter Study of Magnetic Field Strength and Background Temperature
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Integrated temperature perturbation 〈ΔT〉 as a function of nondimensionalized time for simulation sets A1–A5 in Table 1. The circles indicate the maximum of each time series.
Paper: Self-similar Solutions of Oscillatory Reconnection: Parameter Study of Magnetic Field Strength and Background Temperature
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Left column: integrated temperature perturbation 〈ΔT〉 as a function of normalized time. Right column: integrated nondimensionalized ohmic heating as a function of nondimensionalized time. Panels represent simulations with B 0 = 100 G (top), 50 G (middle), and 10 G (bottom), respectively, in Table 1.
Paper: Self-similar Solutions of Oscillatory Reconnection: Parameter Study of Magnetic Field Strength and Background Temperature
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Contour of the ratio of internal energy nondimensionalized by magnetic energy for the initial condition (1 Mm away from the null point). Color bar shows the energy ratio as a function of plasma β 0 and 100E  i0/E  B0.
Paper: Self-similar Solutions of Oscillatory Reconnection: Parameter Study of Magnetic Field Strength and Background Temperature
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Time evolution of the current density at the null point for case D2, j  z (0, 0, t)/j 0, where the × symbol denotes the roots of the function.
Paper: Energy Evolution in the Progenitor of Galaxy Shells: A Semi-analytical Model
Authors: Beibei Guo, Xufen Wu, HongSheng Zhao, Lulu Fan
Figure caption: This figure displays the energy distribution of particles as a function of particle positions (﹩{r}_{i}^{{\prime} }﹩,θ  i ) in the orbital plane of the intruder galaxy on a purely radial orbit (first row, with the same parameters as Model PAR), and nearly radial prograde/retrograde orbits (second/third rows, using the same parameters as Model 3PANR) at the moment of disruption. The energy distributions are shown in polar coordinate systems with the enclosed mass fraction, ﹩f=\tfrac{{M}_{2}({r}_{i}^{{\prime} })}{{M}_{2}}﹩ (where ﹩{M}_{2}({r}_{i}^{{\prime} })={M}_{2}{\left(\tfrac{{r}_{i}^{{\prime} }}{{r}_{s2}}\right)}^{3}/{\left[1+{\left(\tfrac{{r}_{i}^{{\prime} }}{{r}_{s2}}\right)}^{2}\right]}^{1.5}﹩), being the radial coordinates, and the phase angle θ  i  being the azimuthal coordinates. Column 2 depicts the large change in energy distribution from the (almost uniform) initial distribution (column 1), and final distribution (column 3), all expressed as functions of the initial positions of particles on the orbital plane (﹩{r}_{i0}^{{\prime} }﹩,θ  i0). The same change in energy distribution from the initial distribution (column 1) to the final distribution (column 5) is depicted again in column 4, but both are expressed as functions of the positions (﹩{r}_{i}^{{\prime} }﹩, θ  i ) at the epoch of dwarf disruption. Particles that gain the most energy (hollow black circles) and lose the most energy (hollow purple triangles) are marked, as well as particles with the maximum energy E max (solid black circles) and the minimum energy E min (solid purple triangles). In each panel, the five circles, respectively, enclose 10%, 30%, 50%, 70%, and 90% of the total mass of the intruder galaxy.
Paper: Energy Evolution in the Progenitor of Galaxy Shells: A Semi-analytical Model
Authors: Beibei Guo, Xufen Wu, HongSheng Zhao, Lulu Fan
Figure caption: The differential energy distributions n(E)/N of overall (top) and stellar particles (middle) of the intruder galaxy are shown in four snapshots of simulations (at the beginning: blue curve, at T enc = 0 Gyr: cyan, at T enc = 0.1 Gyr: green, at T enc = 2.85 Gyr: orange). These panels correspond to the two N-body models: Models PAR and PIR from the left to right panels. In the two smaller panels appearing in the lower panels, the black line shows the differential energy distribution of all particles n(E) relative to the dwarf galaxy itself at the beginning, while the yellow line represents the stellar particles. The bottom panel shows the comparison of differential energy among the N-body simulation of Model PAR (cyan solid line), the semi-analytical method (gray solid line), and the superposition approach, with the latter two methods having the same parameters for the density profile and orbit as Model PAR, at T enc = 0 Gyr. The lowest energy and the energy of the central particle calculated by the superposition approach are marked as ﹩\min ({E}_{\mathrm{sa}})﹩ and ﹩{E}_{\mathrm{sa}}({r}_{i0}^{{\prime} }=0)﹩, respectively. The energy units of all panels are consistent.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: Comparison between the CCF parameters for the three different models (0G, 3G, uniform) and the data. The values plotted here can be seen in Table 1, for the observed trends in the data, and Table 2 for the three models. The 1σ uncertainties of both the models and data from their corresponding tables are plotted in both of the two top panels, but the model uncertainties are smaller than the size of the markers as these uncertainties are measured on the “zero-noise" model. The top panels shows the peak radial velocity shifts for the beginning of the transit (ϕ −, left) and end of the transit (ϕ +, right) at the three different altitude bins. As the models do not extend to pressures below 10−5 bars, where the strong Fe lines absorb, there are no measurements for the models in the strong-line bin in any of the plots. The middle panels are the same, except instead of radial velocity, they show the measured FWHMs of the CCFs. The bottom panel shows the ratio of the height of the CCFs from the beginning of the transit (ϕ −) divided by the height at the end of the transit (ϕ +).
Paper: Energy Evolution in the Progenitor of Galaxy Shells: A Semi-analytical Model
Authors: Beibei Guo, Xufen Wu, HongSheng Zhao, Lulu Fan
Figure caption: Shows colored orbits of particles of various ICs (top panel) from the intruder galaxy, and their energy E (middle) and angular momentum L  z  (bottom) in the radial collision Model PAR (left panels), and near-radial collision Models 1PANR, 2PANR, and 3PANR (right panels) as functions of the lookback time T enc. The evolution in N-body runs (solid lines) is well matched by our analytical predictions (colored dots).
Paper: Energy Evolution in the Progenitor of Galaxy Shells: A Semi-analytical Model
Authors: Beibei Guo, Xufen Wu, HongSheng Zhao, Lulu Fan
Figure caption: This figure displays the projected densities (upper and second row of panels) of the shell structures formed at T enc = 2.85 Gyr in Models PAR, PIR, HAR, 1PANR, 2PANR, and 3PANR. The phase-space densities (panels in the third row) and the energy densities (bottom panels) of the shell structures formed at T enc = 2.85 Gyr in Models PAR (panels in the left column), 1PANR (panels in the middle column) and 3PANR (panels in the right column) in the N-body simulations. The rainbow and gray color tables illustrate these densities of the stellar and the overall particles of the intruder galaxy, respectively.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption:  K  p -vs.-V wind plots for Fe I (top left), Cr I (top right), V I (bottom left), and Mn I (bottom right). The different colors are overlays of SNR contours for our different altitude bins, and the crosses denote the peak K  p  and V wind value for each altitude bin. The semi-transparent filled contours denote where the SNR has dropped by 1.5 from the peak SNR value, while the line contours of the same color denote where the SNR has dropped by 0.5. In some cases, there are multiple regions of high SNR, which can be seen as multiple contours (see for example the two different navy-blue lined contours for the strong Fe–line bin). We have also used these contours to estimate uncertainties in the peak K  p , which are plotted as error bars on the crosses. We find no clear trend in K  p  offset with altitude.