adsabs/AstroCLIMB huggingface dataset:
Paper: On the Frequency of Multiple Galaxy Mergers in ΛCDM Cosmological Simulations
Authors: Jonathan Mack, Shy Genel
Figure caption: Heatmaps of the time to the second-closest merger versus the time to the closest merger, at the fiducial parameter values (except for Tfac = 2; top) and combined over the full parameter space (bottom). We find that the time until the second-closest merger is typically close to the time to the closest merger, a phenomenon that contributes to the prevalence of multiple mergers.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: Probability density functions (PDFs) of gas velocity (left) and number density (right) in the intergalactic medium (IGM) at z = 20 with and without streaming. The IGM is defined as all gas not inside halos as identified by the FoF. Bottom subpanels show the ratio of the PDFs in each run. While the velocity distributions are nearly identical, indicating that the kinematic imprint of streaming has largely dissipated by this epoch, the number density distribution reveals a suppression of dense filamentary gas (n  ≳  10−1 cm−3) in the streaming run. This difference, integrated over cosmic time, contributes to reduced kinetic energy and turbulence in gas accreting onto halos in the presence of streaming.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: Projected gas density surrounding representative halos from two mass bins in simulations with streaming (bottom rows in each pair) and without streaming (top rows in each pair) at z = 20. Each panel shows a 1 kpc (physical) cutout centered on the halo’s center of mass. The top pair depicts halos with M < 106 M⊙, while the bottom pair depicts halos in the range M = 106–107 M⊙. White circles denote the virial radius of each halo. Low-mass halos appear similarly isolated in both streaming and no-streaming runs and are embedded along thin filaments. In contrast, higher-mass halos without streaming reside in denser environments with more frequent filamentary intersections and nearby structures, conditions favorable for mergers. This visual difference suggests that streaming may suppress merger-driven turbulence in high-mass halos by reducing the abundance of dense nearby structures.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: Shocked gas in an illustrative halo of mass M ≃ 107 M⊙ at z = 20. Top panel: All gas within the halo is shown in gray, while shocked gas is overplotted in blue. Red arrows indicate normalized velocity vectors of shocked gas outside the virial radius of the halo, and yellow arrows indicate those inside. The dashed green circle marks the virial radius. We see that the shocked gas predominantly traces radially oriented accretion shocks. Bottom panel: Gas temperature distribution, where shocked gas is outlined in black. Shocked gas reaches temperatures near the virial temperature, consistent with strong thermalization during accretion.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: Percent difference in turbulent velocity between streaming (vbc = 1σvbc, vbc = 2σvbc, vbc = 3σvbc) and no-streaming (vbc = 0σvbc) simulations as a function of total halo mass. Shaded color bands indicate the 1σ uncertainties, computed via standard error propagation of the ratio of means. The percent difference is computed separately in each mass bin. The enhancement of turbulence grows with increasing streaming for low-mass halos (M ≲ 106 M⊙), while turbulence is suppressed at higher masses across all streaming strengths.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: Gravitational potential energy of halos as a function of total mass (gas + DM) at z = 20 with and without streaming. The top panel shows the halo’s gravitational potential energy, computed from gas–gas, DM–DM, and gas–DM interactions for all gas cells and dark matter particles within each halo. The green dashed line shows the expected scaling of slope 5/3 for virialized halos. Shaded color bands indicate the 1σ scatter around the mean values. The bottom panel shows the ratio of the two curves. No-streaming halos exhibit systematically higher potential energies across the full mass range.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: Turbulent Mach number as a function of total halo mass with and without streaming at z = 20. Shaded color bands indicate the 1σ scatter around the mean values. A clear turnover appears near M ∼ 106 M⊙, marked by a gray band, mirroring the trend in the turbulent velocity (Figure 1). Horizontal gray line marks a Mach number of 1.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: RMS and turbulent velocities as a function of halo mass in the higher-resolution run. Shaded color bands indicate the 1σ scatter around the mean values. The turnover in turbulence remains at M ∼ 106 M⊙, marked by the gray shaded band, while the difference between streaming and no-streaming begins to saturate for the lowest-mass halos.
Paper: Supersonic Turbulence in Primordial Halos: a Comparison with and without the Stream Velocity
Authors: Avi Chen, William Lake, Claire E. Williams, Blakesley Burkhart, Smadar Naoz, Shyam H. Menon, Federico Marinacci, Mark Vogelsberger, Naoki Yoshida
Figure caption: Average energy dissipation rate from shocked gas as a function of total halo mass at z = 20. Shaded color bands indicate the 1σ scatter around the mean values. At high-mass halos (M  ≳  106 M⊙), no-streaming halos exhibit higher dissipation rates, consistent with enhanced energy in accretion flows.
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: Same as Figure 1 but with disk fluxes scaled by the stellar luminosities. Our model radii for USco disks (detailed in the text) are shown as solid blue circles. These are typically much smaller than the values from N. Hendler et al. (2020). The gray line is the theory prediction for disks that remain optically thick throughout (at 3 mm) and are viewed at an inclination of 60∘ (see Appendix A). The Lupus sample suggests that almost all disks are optically thick, with the exception of the largest ones. The same conclusion also holds for the USco disks, if we adopt our model radii. Colored contours are kernel density estimates of disks in Lupus and USco (using our model radii).
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: Disk fluxes versus disk sizes, compiled from literature (see the text for references). The disk radii enclose 68% of the total flux. All fluxes are at 0.88 mm and are calibrated to a distance of 140 pc. The orange line represents the SLR obtained by S. M. Andrews et al. (2018) for large disks in Lupus: Lmm = 0.05 mJy (R/au)2. Most disks appear to obey this trend (L ∝ R2), except for the USco disks. The Lupus sample (73 disks) has a median resolution of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩04 (∼6 au); while the USco sample (21 disks) has a worse median resolution at ﹩0\mathop{.}\limits^{^{\prime\prime} }37﹩ (∼58 au).
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: Dust opacities (per gram of dust mass) for power-law grain size distributions, dN/da ∝ a−3.5 at the left and a−2 at the right, at two observing wavelengths and plotted against the maximum grain sizes. The solid lines represent the total opacity, while the dotted and dashed represent that of absorption (﹩{\kappa }_{\lambda }^{{\rm{abs}}}﹩) and scattering (﹩{\kappa }_{\lambda }^{{\rm{scat}}}﹩) components, respectively. Scattering dominates for grain sizes of interest (100 μm to cm). The value of ﹩\beta =d\mathrm{ln}\kappa /d\mathrm{ln}\lambda ﹩ depends on the size distribution, being nearly zero for the right panel when ﹩{a}_{{\rm{\max }}}﹩ is beyond 1 mm.
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: Evolutionary tracks in the bulk properties (flux, R68%, and α1−3) of smooth disks, for the same models as in Figure 6 but with Rd initialized at 5, 10, 20, and 50 au. The contours and the black line are the same as in Figures 2 and 3. Without bouncing, all disks turn optically thin and dim down quickly. It is difficult to maintain these disks near the observed values. Bouncing allows most disks to lie on the observed SLR for megayears, as well as maintaining small values of α1−3. The most compact disks do observe a moderate rise in α1−3. This results from a reduction in the optical depth by viscous spreading and grain drain.
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: Radial profiles of an evolving disk under different conditions: the two left columns experience different α and no bouncing; the right column is subject to the bouncing barrier. The disk has an initial density profile that is cutoff at Rd = 20 au (Equation (1)). Colored curves show snapshots taken at t = 0, 0.03, 0.5, 1 and 3 Myr. Top row: surface densities of gas (dashed curves) and dust (solid); second row: maximum (solid) and mass-averaged (dashed) grain sizes—we estimate the maximum one at the top 2.1% (2σ) of the mass density; third row: Stokes number for ﹩{a}_{{\rm{\max }}}﹩; bottom row: vertical optical depth (τ3mm), with the short vertical ticks denoting R68%. Without bouncing, grains grow and drain rapidly, and the disks turn optically thin within 1 Myr. Bouncing stalls grain growth at ∼100 μm. This slows down grain drain and the disk remains optically thick and stays at roughly the same size for a few megayears.
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: The dependency of the spectral index on the optical thickness at the disk outer edge, τ3mm(r = Rd). The default dust population (thick black curve) have a maximum size of ﹩{a}_{{\rm{\max }}}=100\,\mu {\rm{m}}﹩ and a power-law exponent of apow = 3.5. Other solid curves show different values of ﹩{a}_{{\rm{\max }}}﹩, while the dashed group repeat with apow = 2. To reproduce the observed distribution of α1−3 (right histogram), one either requires optically thick disks (with any ﹩{a}_{{\rm{\max }}}﹩), or optically thin disks with a dust population that is nearly monodisperse (low apow) and large (>1mm).
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: A cartoon illustrating the three regimes of collision outcomes, emulating those in C. Güttler et al. (2010) and C. Dominik & C. P. Dullemond (2024). The regimes are separated by the bouncing and fragmentation thresholds (between two equal-sized grains), as in Equations (6) and (4). The two lines represent relative encounter velocities, from turbulent stirring, Vα (assuming α = 10−4; solid curve) and from differential radial drift, ΔVdrift (between grains a factor of 2 in size; dashed curve). These values are evaluated for our default disk at 20 au. In the presence of bouncing, grain growth is truncated at a small size, abounce ∼ 100 μm, rather than the much larger afrag.
Paper: Bouncing Grains Keep Protoplanetary Disks Bright
Authors: Yansong Qian, Yanqin Wu
Figure caption: Spectral indexes for disks from Lupus (M. Tazzari et al. 2021b) and USco (this work), plotted against the scaled disk fluxes. USco disks are dimmer than those in Lupus but have similarly low spectral indexes.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: The left panel shows the distribution of the r-band magnitude as a function of redshift. The red stepped solid lines indicate that the 95th percentile in each redshift bin is adopted as the magnitude limit (﹩{m}_{{r}_{{\rm{lim}}}}﹩). The right panel displays the distribution of stellar mass as a function of redshift. The corresponding stellar-mass-complete limit (Mcomp) for each bin is derived from the magnitude limit and is depicted as the red stepped solid line. Meanwhile, the overall 90% mass-complete cutoff across the redshift range, derived via interpolation of these binned values, is denoted by the black dashed–dotted line (with black triangular markers at the interpolated data points).
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: The contour plot illustrates the size–mass distribution in logarithmic space. The red and blue contours show the distributions of RDGs and BDGs in different redshift bins, respectively. The red dotted line and blue solid line represent the size–mass relations of RDGs and BDGs derived from the best-fit model in the corresponding redshift bins. For comparison, we plot the best-fit lines of RDGs and BDGs in the same redshift bin. The top left corner shows the total sample size for the corresponding redshift bin. The bottom right corner displays the slope of the best-fit line, with the error value calculated as the standard error of the residuals between the actual data and the linear model, taking into account the weights of outliers.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: The contour plot shows the size–mass distribution in logarithmic space. The top four subplots represent RDGs, while the bottom four subplots represent BDGs. The green dotted contour lines depict the distribution of disk galaxies in the field environment, while the blue solid contour lines show their distribution in the cluster environment. The corresponding straight lines represent the size–mass relations for each environment. The number in the upper left corner indicates the number of galaxies in the bin, while the number in the lower right corner represents the slope value of the size–mass relation for the field or cluster galaxies in the bin. The error value is calculated as the standard error of the residuals between the actual data and the linear model, taking into account the weights of outliers.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: The cumulative distributions of the logarithmic stellar mass and the half-light radius are shown in the top and bottom panels, respectively. The red solid line represents RDGs in clusters, the green dotted–dashed line represents BDGs in clusters, the magenta dashed line represents RDGs in the field, and the blue dotted line represents BDGs in the field.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: The contour plot and size–mass distribution in logarithmic space of the mass-matched subsample (cluster:field = 1:3). The annotations in the figure are similar to those in Figure 5.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: Cumulative distribution functions for the radial distances of RDGs and BDGs in galaxy clusters at different redshifts. The thicker dark lines (red, orange, green, and blue) represent cluster RDGs across the four redshift bins, while the corresponding thinner light lines (salmon, gold, spring green, and dodger blue) represent cluster BDGs. The different line styles (solid, dashed, dotted–dashed, and dotted) represent the cumulative distribution functions of galaxy samples at four different redshifts. The corresponding vertical lines in the figure represent the median radial distances for different subsamples.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: Contour plot of the size–mass distribution for RDGs in logarithmic space. The lines show the best-fit size–mass relations for galaxies in different local density environments (Σ10): low (green dotted; <16th percentile) and high (blue solid; >84th percentile) density. The contours of corresponding colors represent the sample distribution. The numbers in the top left and bottom right corners of each panel indicate the galaxy count and the slope of the best-fit line ± its standard error, respectively.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: The contour plot and size–mass distribution in logarithmic space of the mass-matched subsample (RDGs: BDGs = 1:3). The annotations in the figure are similar to those in Figure 3.
Paper: Environmental Effects and Size–Mass Relations of Red Disk Galaxies at 0.1 < z < 0.5
Authors: Zhaobin Chen, Yizhou Gu, Hu Zou, Qirong Yuan
Figure caption: Comparison of effective radii from GALFIT (x-axis) and the DESI Tractor pipeline (y-axis). Points are color-coded by their deviation from the one-to-one line: blue for within 1σ, red for beyond. The legend gives the standard deviations for the full sample and the 1σ subset.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: NuSTAR FPMB light curves for all six epochs combined (top panel) and plotted separately (lower panels). All the light curves have been binned to 100 s. For Epoch 5, the dashed horizontal line separates the persistent interval from the dip interval.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: The residuals from joint fits to the data from Epochs 1–6 using both phenomenological and physical models. The data points shown are from FPMB. In all cases, only data from the persistent spectra are considered for Epoch 5.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Comptonized disk blackbody model fit to data from all six epochs using the model cons*TBabs*simplcut*diskbb. Relativistic reflection features are evident in all six epochs. For Epoch 5, only the persistent spectra are plotted.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Evolution of the photon index Γ and the corona temperature kTe with the 2–10 keV flux for all six NuSTAR epochs. The 2–10 keV flux decreased monotonically from Epoch 1 to Epoch 6. We note that the uncertainties on the fluxes are plotted but very small.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Energy-resolved light curve for Epoch 5.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Exposure-corrected NuSTAR image of IGR J17091−3624 from Epoch 4 (the color map is logarithmically scaled). The source and background regions, each extracted from a 100″ radius, are captured by the white and red circles, respectively. The color scale of the image is in counts per pixel. The horizontal and vertical axes are the J2000 coordinates of the system.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Left: PDS of the six NuSTAR epochs, shown in units of fractional rms squared. The variability above ∼2 Hz is consistent with zero. Right: PDS of Epoch 5, extracted during the full interval, persistent phase, and dip intervals of the light curve. In both panels, the Poisson noise level was estimated by averaging the power above 100 Hz and subtracted across all frequencies.
Paper: The 2025 Failed Outburst of IGR J17091−3624: Spectral Evolution and the Role of Ionized Absorbers
Authors: Oluwashina K. Adegoke, Javier A. García, Guglielmo Mastroserio, Elias Kammoun, Riley M. T. Connors, James F. Steiner, Fiona A. Harrison, Douglas J. K. Buisson, Joel B. Coley, Benjamin M. Coughenour, Thomas Dauser, Melissa Ewing, Adam Ingram, Erin Kara, Edward Nathan, Maxime Parra, Daniel Stern, John A. Tomsick
Figure caption: Left: best fit to the persistent spectra of Epoch 5 using the model cons*TBabs(simplcut*diskbb+relxillCp) with the dip spectra overlaid. Right: overall best fit to the joint persistent and dip spectra employing the model cons*TBabs*XSTAR(simplcut*diskbb+relxillCp).