adsabs/AstroCLIMB huggingface dataset:
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: The R − z plane projections of three orbits from the SoS shown in Figure 1. The gray (untrapped) orbit corresponds to the gray contour just inside the smaller branch of the separatrix, and the orange (trapped) orbit corresponds to the larger of the two orange contours in the upper resonant island. The black orbit corresponds to the 1:1 commensurable orbit that parents the trapped orbit family at the 1:1 resonance, represented by the upper black cross in Figure 1. No member of the trapped orbit family parented by this commensurable orbit will fill the top left or bottom right areas of the plot like the untrapped orbit does.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: The mock ALMA tSZ maps at 320 GHz (Band 7) for different feedback modes around the most massive and most active BHs at two different redshifts from Davé et al. (2019) using the observational parameters in Table 3. Top panel: mock ALMA tSZ maps for the no-feedback (leftmost column), no-jet feedback, no X-ray feedback, and all-feedback modes (rightmost column), respectively, around the most massive BH at z ∼ 1. Second panel: mock ALMA tSZ maps for the no-feedback, no-jet feedback, no X-ray feedback, and all-feedback modes, respectively, around the most active BH at z ∼ 1. Third panel: same as the top panel but now at z = 0.016. Fourth panel: same as the second panel but now at z = 0.016. We note that ALMA has the capability to detect the SZ signal for the no-feedback and no-jet feedback modes. The signal gets enhanced when only the radiative mode of feedback is added. For the no X-ray feedback and all-feedback modes, the signal gets suppressed below the noise threshold of ALMA. The different feedback models and the BH properties are summarized in Tables 1 and 2 respectively. The ALMA results are summarized in Table 4.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: The theoretical simulated tSZ maps for different feedback modes (leftmost: no feedback, second left: no jet feedback. Second right: no X-ray feedback, rightmost: all feedback) around similar BHs at z ∼ 1 from D19). Top panel: simulated tSZ map at 320 GHz of the most massive BH for the no-feedback, no-jet feedback, no X-ray feedback, and all-feedback modes, respectively. Bottom panel: same as the top panel but now for the most active BH. From the figure, we can see that the addition of radiative feedback and jet feedback have opposing effects (enhancement vs. decrement) in the SZ signal. Tables 1 and 2 summarizes the feedback model nomenclature and the BH properties, respectively.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: Same as in Figure 1 but at z = 0.016. Top panel: simulated tSZ map at 320 GHz of the most massive BH for the no, no-jet, no X-ray, and all-feedback modes, respectively. Bottom panel: same as the top panel but now for most active BHs. Tables 1 and 2 summarize the feedback model nomenclature and the BH properties, respectively. The results are the same as those shown in Figure 1 for the high redshift BHs. The inclusion of the radiative mode of feedback enhances the SZ signal while adding the jet mode decreases it. This is in stark contrast to the X-ray signal where both modes suppress the X-ray flux (see Kar Chowdhury et al. 2022)
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: The fidelity (S/N) maps of the mock ALMA tSZ simulations at 320 GHz for different feedback modes around the most massive and the most active BHs at two different redshifts from D19 corresponding to Figure 4. Top panel: fidelity maps for the no-feedback, no-jet feedback, no X-ray feedback, and all-feedback modes, respectively, around the most massive BH at z ∼ 1. Second panel: mock ALMA tSZ maps for the no-feedback, no-jet feedback, no X-ray feedback, and all-feedback modes, respectively, around the most active BH at z ∼ 1. Third panel: same as the top panel but now at z = 0.016. Fourth panel: same as the second panel but now at z = 0.016.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: Simulated ALMA maps constructed using the same observing parameters as Figure 4 but at 135 GHz (Band 4, leftmost column), 100 GHz (Band 3, middle column), and 42 GHz (Band 1, rightmost column) for the most massive high redshift (z = 1) BH. Top panel: mock ALMA tSZ maps for no feedback Second panel: the corresponding S/N maps, Third panel: same maps, but now for the no-jet feedback mode. Fourth panel: the S/N maps corresponding to the third panel. The signal is enhanced when we have radiative feedback from the BHs.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: The theoretical SZ radial profiles of the most massive and most active BHs corresponding to Figures 1 and 2. Top left: radial profile for the most massive BH for the no, no-jet, no X-ray, and all-feedback modes, respectively, at z ∼ 1 (see Table 1 for nomenclature and Table 2 for BH properties). Top right: same as the upper left panel but now at z = 0.016. Bottom left: same for the most active BH at z ∼ 1. Bottom right: same as the lower left panel but now at z = 0.016. We note that for all four cases, we hardly see any significant difference between no feedback and no-jet feedback modes but no X-ray feedback and all-feedback modes are separable. A significant suppression of the signal occurs when the jet mode of feedback is introduced in the model.
Paper: Disk Wind–Driven Expanding Radio-emitting Shell in Tidal Disruption Events
Authors: Kimitake Hayasaki, Ryo Yamazaki
Figure caption: Comparison of the radial profile of the ambient matter density (panel (a)) and the shell radius evolution (panel (b)) between our model and the observed data of AT 2019dsg (Cendes et al. 2021). In panel (a), the red filled circles with error bars and the solid black line depict, respectively, the observed data and the radial density profile, which is given by Equation (10). The vertical and horizontal axes indicate the ambient matter density normalized by ρ ej,0 and the radius normalized by r 0, respectively. In panel (b), the solid red and black lines denote the free expansion and numerical solutions, respectively. The blue filled circles with error bars depict the observed data. The vertical and horizontal axes denote R(t)/r 0 and (t + T d)/t 0, respectively, where T d is the onset time of OUV emissions (see also Equation (38) and Table 1). The set of parameters (n, s, ϵ, η, δ) = (5/3, 2.1, 2.0, 0.028, 5.0) is adopted for the numerical solution, R(t).
Paper: Disk Wind–Driven Expanding Radio-emitting Shell in Tidal Disruption Events
Authors: Kimitake Hayasaki, Ryo Yamazaki
Figure caption: Time evolution of the shell radius.  Panels (a)–(e) depict the dependence of the shell radius evolution on δ, η, s, n, and ϵ, respectively. In all panels, the dashed lines denote the shell radius evolving by free expansion, y − y 0 = (x − x 0)/ϵ. The different colors represent the different values of each parameter.
Paper: Disk Wind–Driven Expanding Radio-emitting Shell in Tidal Disruption Events
Authors: Kimitake Hayasaki, Ryo Yamazaki
Figure caption: Comparison of the dimensionless expanding shell radius y(x) between analytical and numerical solutions for different parameters.The vertical and horizontal axes denote y − y 0 and x − x 0, respectively, where y = R(t)/r 0, y 0 = 1, x = t/t 0, and x 0 = 1. In each panel, the solid black line represents the numerical solution of the shell radius, while the red and blue dashed lines show the approximate solutions given by Equation (25) up to the second and third orders, respectively.
Paper: Disk Wind–Driven Expanding Radio-emitting Shell in Tidal Disruption Events
Authors: Kimitake Hayasaki, Ryo Yamazaki
Figure caption: Time evolution of the local power-law index of time for the shell radius. Panels (a)–(e) represent the dependence of the power-law index evolution on δ, η, s, n, and ϵ, respectively. The different colors show the different values of each parameter.
Paper: Disk Wind–Driven Expanding Radio-emitting Shell in Tidal Disruption Events
Authors: Kimitake Hayasaki, Ryo Yamazaki
Figure caption: Time evolution of the expanding shell. Panels (a), (b), (c), and (d) represent the time evolution of the shell radius, the shell mass, the mass addition rate to the shell, and the force acting on the shell, respectively (see Section 3.1 for the detailed formats). Note that the force curve is drawn by ∣F∣ = ∣F ej − F am∣ because F am > F ej. We adopt the set of parameters (n, s, ϵ, η, δ) = (5/3, 1.0, 1.0, 1.0, 1.0) as the fiducial model.
Paper: Disk Wind–Driven Expanding Radio-emitting Shell in Tidal Disruption Events
Authors: Kimitake Hayasaki, Ryo Yamazaki
Figure caption: Time evolution of the power-law index of time, m, for the shell radius (see Equation (29)) with the fiducial parameters (n, s, ϵ, η, δ) = (5/3, 1.0, 1.0, 1.0, 1.0). The dashed black and green lines represent the free expansion (m = 1) and asymptotic (m = 1/(4 − s)) solutions, respectively, whereas the solid black line denotes the evolution of m.
Paper: Choked Jets in Expanding Envelope as the Origin of the Neutrino Emission Associated with Tidal Disruption Events
Authors: Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The accumulative neutrino numbers (the color map) as a function of the jet luminosity and bulk Lorentz factor assuming envelope masses of three TDEs given in Case A. The white solid lines represent the parameter values corresponding to the minimally required neutrino numbers, which are N  ν  = 0.008 for AT2019dsg and N  ν  = 0.007 for AT2019fdr and AT2019aalc (Stein et al. 2021; Reusch et al. 2022). The white dashed line represents the critical parameter values for jets being choked and the direction of the arrow means that the permitted parameter space for choked jets is below this line. Red crosses mark the points in the parameter space that were chosen to produce the results in Figures 4 and 5. The top and bottom panels represent the cases of n = 3 and n = 2 for the envelope density profile, respectively. Internal shock radius are taken to be R int = 3 × 1014 cm for AT2019aalc and AT2019fdr, and R int = 1014 cm for AT2019dsg. α = 5/3, β = 5/12, θ j,0 = 1/3 and f ph = 0.05 are used in the calculation. Other parameters are listed in Table 2.
Paper: Choked Jets in Expanding Envelope as the Origin of the Neutrino Emission Associated with Tidal Disruption Events
Authors: Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Upper panel: Neutrino spectra of three TDE events in Case A. The jet luminosities are taken to be L j,0 = 1044 erg s−1 for AT2019dsg, L j,0 = 5 × 1045 erg s−1 for AT2019fdr, and L j,0 = 8 × 1044 erg s−1 for AT2019aalc. Lower panel: Neutrino spectra of three TDE events in Case B. The jet luminosities are taken to be L j,0 = 3 × 1044 erg s−1 for AT2019dsg, L j,0 = 3 × 1045 erg s−1 for AT2019fdr, and L j,0 = 5 × 1044 erg s−1 for AT2019aalc. The solid and dotted–dashed lines represent the neutrino spectra in the n = 3 and n = 2 profiles, respectively.
Paper: Choked Jets in Expanding Envelope as the Origin of the Neutrino Emission Associated with Tidal Disruption Events
Authors: Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Time evolution of cumulative neutrino numbers. The symbols and parameter values are identical with those in Figure 4.
Paper: Choked Jets in Expanding Envelope as the Origin of the Neutrino Emission Associated with Tidal Disruption Events
Authors: Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The schematic picture of a choked TDE jet in an expanding envelope. A quasi-spherical envelope surrounding the black hole is expanding outwardly with a velocity of ∼104 km s−1. Jet is collimated by the cocoon pressure to a cylinder shape and it is choked inside the envelope. Internal shocks (yellow wavy lines) occurred within the jet accelerate cosmic-ray protons, which produce neutrinos observed by us.
Paper: Choked Jets in Expanding Envelope as the Origin of the Neutrino Emission Associated with Tidal Disruption Events
Authors: Jian-He Zheng, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Same as Figure 2, but using the envelope masses of three TDEs given in Case B.
Paper: SN 2020bio: A Double-peaked, H-poor Type IIb Supernova with Evidence of Circumstellar Interaction
Authors: C. Pellegrino, D. Hiramatsu, I. Arcavi, D. A. Howell, K. A. Bostroem, P. J. Brown, J. Burke, N. Elias-Rosa, K. Itagaki, H. Kaneda, C. McCully, M. Modjaz, E. Padilla Gonzalez, T. A. Pritchard, N. Yesmin
Figure caption: The full extinction-corrected light curves of SN 2020bio. Photometry in different filters have been offset for clarity. Unfiltered photometry from the Itagaki Astronomical Observatory is included as clear points and calibrated to the V band. The inset focuses on the rapidly evolving shock-cooling emission.
Paper: Neutrino-driven Winds in Three-dimensional Core-collapse Supernova Simulations
Authors: Tianshu Wang, Adam Burrows
Figure caption: Nucleosynthesis yields and production factors (the ratio of the calculated abundances and solar abundances) in the winds. Top: mass fraction at the end of six representative simulations. Bottom: production factors at the end of those simulations. The production factor is calculated based on the solar system abundances given in Lodders (2021). Isotopes with the same mass number (A) are summed together in both panels. Some interesting isotope positions are indicated at the top of each panel. This figure confirms that the winds are able to generate heavy isotopes up to the 90Zr peak, thanks to the weak r-process and the ν p-process. However, the 9.5 and 23 M ⊙ models do not generate as many heavy elements. One reason is that they have very little neutron-rich ejecta and therefore do not experience any significant r-process. Another reason is that the ν p-process (included in this study) can generate heavy elements only if the wind terminates neither too early nor too late (Arcones & Thielemann 2013), which is probably not satisfied by these models. This means that the ν p-process will be sensitive to the morphology of the winds and the explosion. We therefore conclude that it is difficult to predict ν p-process yields without doing actual 3D simulations.
Paper: Neutrino-driven Winds in Three-dimensional Core-collapse Supernova Simulations
Authors: Tianshu Wang, Adam Burrows
Figure caption: Angular mass distributions of the wind and all ejecta at the end of the simulation for the 9.25, 11, and 17 M ⊙ models. Left: wind ejecta. Right: all ejected matter (all matter with a positive binding energy) at the end of the simulations; the outer stellar envelopes not on our grids are not included. It can be seen that on larger angular scales the winds are generally distributed along the same directions as the explosion, while on smaller scales they are much less correlated with the distribution of the total ejecta. This is because the winds are more associated with the high-velocity, high-entropy, low-density bubbles.
Paper: Neutrino-driven Winds in Three-dimensional Core-collapse Supernova Simulations
Authors: Tianshu Wang, Adam Burrows
Figure caption: Electron fraction vs. entropy of the tracer particles during the acceleration phase. Color shows the mass at a given Y  e  and entropy. Y  e  = 0.5 is marked as a vertical white dashed line. Only wind matter is shown here. The fact that wind matter is at most moderately neutron-rich and does not have high enough entropy eliminates the possibility of a strong r-process. However, a weak r-process is allowed, as expected by Wanajo (2013), Arcones & Thielemann (2013), and Wanajo (2023) and seen in this study (see Figure 12).
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: The zoomed-in view of the model galaxy and its surroundings at z = 0. Here, the views of all panels are oriented to show the edge-on view of the satellite plane. From panel (a) to panel (e), the upper right panel shows the image of the central spiral galaxy of the model halo (halo395). Panel (b) shows the distribution of all luminous satellites (M ⋆ > 105 M ⊙), and the top 14 brightest satellites are marked by white filled circles. The central cyan filled circle indicates the central stellar disk, which is almost perpendicular to the satellite plane. Panel (c) shows a “M31” analog (M 200 = 5.2 × 1011 M ⊙). The “Centaurus A/M83 group” (with halo mass M 200 = 1.4 × 1013 M ⊙) is shown as big circle in panel (d) where the points represent all subhalos with M ⋆ > 108.5 M ⊙. Panel (e) shows the large-scale environment around the model galaxy. The dotted circles in each panel are scaled by the virial radius of the halos in that panel. The whiteness of points in each panel are scaled to the stellar mass of the satellites. The thickness of the slices in (e) and (d) are 3 cMpc and 8 cMpc, respectively, where cMpc is the comoving units.
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: Edge-on view of the satellite plane of halo395 and MW. This figure is for satellite plane problem, which shows the positions of the top 14 brightest model/MW satellites (blue/red stars) and central stellar disk (thick black solid line). The view is oriented to show the edge-on view of both the central stellar disk and the satellite plane (long black solid line). Color blue/red indicate that satellites are moving out of/into the screen. The long black dashed lines indicate the rms height of the plane (Section 2). The left/right panels depict halo395/MW.
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: The  k –Δ  k   curve. Yellow data points with error bars show the observational results of the MW with 1σ uncertainty. The magenta triangles are for the model galaxy, halo395.
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: The  k –θ   k   relation. Yellow data points with error bar show the observational result of the MW with 1σ uncertainty and magenta triangles for the model galaxy. Here θ  k  is the angle between the average of the satellite angular momentum and the normal of the satellite plane. This quantity measures how well the orbital plane is aligned with the spatial plane.
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: The satellites radial distribution of MW and halo395. The black dashed line with gray shaded region shows the observational result of MW with 1σ uncertainty, and the orange solid line is that of halo395. Apparently, the satellites radial distribution of halo395 broadly match the observation.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: The peculiar velocity map (top left), the FWHM map (top right), and the S/N([O III] λ5007) map (bottom middle). The bins are obtained via our adaptive binning algorithm with a target S/N of 10 for the [O III] λ5007 line. For saturated regions, we simultaneously fit the strong emission lines, [O II] λ λ3726, 3729, Hβ, Hγ, Hδ, and [O III] λ4959, to find the peculiar velocity or FWHM. Instead, we only fit the [O III] λ5007 line in the unsaturated regions. Top left: bins with S/N(v  p ) < 3 have been masked out. Each bin is color coded by its own v  p . The bins with a reddish color mean they have values of v  p  larger than 5 km s−1. The bins with a bluish color mean they have values of v  p  less than −5 km s−1. The bins with black color represent they have values of v  p  ranging from −5 km s−1 to 5 km s−1. The position of each stellar association is marked the same as in Figure 1. Top right: following the same binning procedure, each bin has S/N(v  p ) ≥ 3. Each bin is color coded by its own FWHM value in velocity space. The white square regions with labels “E1,” “E2,” and “E3” represent the blueshifted, zero-velocity, and redshifted regions, respectively, in Figure 6. Bottom middle: each bin is color coded by the S/N of the [O III] λ5007 line. For each panel, the photometric major axis is shown as a gray dashed line. To determine the major axis, the background-subtracted r-band DECalS image (see Section 2.3) is fitted using a 2D Gaussian function that aligns with the second-order moments of the source before the deblending process, implemented with Photutils. The estimated inclination of this source from Photutils is ﹩i={\cos }^{-1}(b/a)\approx 60^\circ ﹩.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: Variations in the [O III] λ5007 line profiles along the minor axis around the PSB region. The [O III] λ5007 line is extracted from the E1 or blueshifted (left), E2 or zero-velocity (middle), and E3 or redshifted (right) regions, respectively, in Figure 5. Only the double-Gaussian fitting is shown in each panel. In the panels for E1 and E3, the redshift and blueshift components are respectively represented by blue and cyan dashed lines. For E2, the broad and narrow components correspond to the dashed and cyan dashed lines, respectively. Their summation is shown as a red dashed line. The vertical gray dashed line represents the systemic velocity. The reduced χ 2 values for the single- and double-Gaussian fittings are listed at the upper right corner of each panel. The high absolute peculiar velocities in regions E1 and E3 are associated with an unresolved second velocity component confirmed by the F-test (Section 2.5). These two velocity components result in asymmetric line profiles and large FWHM values. In the context of a biconical morphology, each component is generated by the front and back sides of the outflow, respectively. The F-test results for E2 suggest the requirement for a second (broad) velocity component. The broad component, indicative of turbulent outflowing gas, originates from the PSB (or the outflow launching) region. Because this broad component shares a velocity centroid similar to the narrow component, it does not significantly impact the line profile to increase its FWHM.