adsabs/AstroCLIMB huggingface dataset:
Paper: Linking Electron Density with Elevated Star Formation Activity from z = 0 to z = 10
Authors: Sijia Li, Si-Yue Yu, Luis C. Ho, John D. Silverman, Jing Wang, Amélie Saintonge, Niankun Yu, Qinyue Fei, Daichi Kashino, Hao-ran Yu
Figure caption: Relations between the [S II] doublet ratio ([S II] λ6716/λ6731), ne, and line width (σ[S II]) with various galaxy properties. Gray dots represent individual galaxies, while black points with error bars indicate the median and scatter in each bin. In the ne–ΣSFR panel, black points show the median ne derived from the median line ratio, with error bars denoting the uncertainties of the median; the best-fit broken power law is shown in blue. Circles in this panel mark the median values for galaxies with S/N > 10 in all emission lines used. In the Mtotal–SFRtotal and Σ*–ΣSFR panels, the color scale encodes the median line ratio in each bin, and bins with fewer than five galaxies are omitted.
Paper: Linking Electron Density with Elevated Star Formation Activity from z = 0 to z = 10
Authors: Sijia Li, Si-Yue Yu, Luis C. Ho, John D. Silverman, Jing Wang, Amélie Saintonge, Niankun Yu, Qinyue Fei, Daichi Kashino, Hao-ran Yu
Figure caption: Relationship between ne and ΣSFR. Our low-redshift measurements and the corresponding best-fit relation are shown as blue points and a blue curve. High-redshift measurements (z = 0.9–10.2) from previous studies are overplotted (C. C. Steidel et al. 2014; R. Shimakawa et al. 2015; R. L. Sanders et al. 2016a, 2016b; M. Kaasinen et al. 2017; D. Kashino et al. 2017; R. L. Davies et al. 2021; N. A. Reddy et al. 2023a, 2023b; Abdurro’uf et al. 2024; S. Fujimoto et al. 2025; M. W. Topping et al. 2025).
Paper: Linking Electron Density with Elevated Star Formation Activity from z = 0 to z = 10
Authors: Sijia Li, Si-Yue Yu, Luis C. Ho, John D. Silverman, Jing Wang, Amélie Saintonge, Niankun Yu, Qinyue Fei, Daichi Kashino, Hao-ran Yu
Figure caption: Basic properties of our galaxy sample. From left to right, the panels present the histogram of redshift (z), axis ratio (q), the diagram of Mtotal versus SFRtotal, and the BPT diagram of [O III] λ5007/Hβ versus [N II] λ6584/Hα. The straight line represents the star-forming main sequence for galaxies at z ≤ 0.04, and the contours indicate regions enclosing a given fraction of the galaxies in the parent sample. The solid curve in the BPT diagram marks the empirical separation between star-forming galaxies and AGNs, as defined by G. Kauffmann et al. (2003).
Paper: Linking Electron Density with Elevated Star Formation Activity from z = 0 to z = 10
Authors: Sijia Li, Si-Yue Yu, Luis C. Ho, John D. Silverman, Jing Wang, Amélie Saintonge, Niankun Yu, Qinyue Fei, Daichi Kashino, Hao-ran Yu
Figure caption: Redshift evolution of ne. The open circles mark the ne evolution, derived from our ne–ΣSFR relation for a fixed stellar mass of 5 × 1010 M⊙ combined with the redshift evolution of ΣSFR. The black curve represents the best-fit function, ne = 40 × (1 + z)1.4 cm−3. The gray shaded area shows the range estimated by Y. Isobe et al. (2023), while the dotted, dashed, and dashed–dotted lines indicate trends from Abdurro’uf et al. (2024), M. W. Topping et al. (2025), and S. Li et al. (2025), respectively.
Paper: A 50 minute Coronal Kink Oscillation and Its Possible Photospheric Counterpart
Authors: Sihui Zhong, Valery M. Nakariakov, Dmitrii Y. Kolotkov
Figure caption: Temporal variation of mean BLoS in ROI1. (a) The footpoint region (ROI1) of the loop of interest is seen in the HMI LoS magnetogram. (b) Time series of average LoS magnetic field in ROI1. The red dashed lines indicate the time duration of the observed 50 minute kink oscillations. The blue lines indicate the selected time interval where the 50 minute periodicity is detected by EMD analysis. The blue curve is the trend of the selected signals. (c) The detrended time series (black) is overlaid with the detected EMD mode 6 (red). (d) Wavelet spectrum of the mean magnetic field in ROI1 from 12:45 to 19:00 UT. The global normalized spectrum (blue) and the 95% confidence level (red) are shown on the right of the wavelet spectrum. (e) EMD energy spectrum of the selected signals. The vertical dotted line indicates the threshold of detectable periodicity. (f) Hilbert spectrum of the EMD mode 6 shows the instantaneous period’s time evolution. The red curve represents the values with maximum power. The dotted line indicates 50 minute periodicity. (g) The trajectory of the centroid position of the loop footpoint. The color scheme from dark purple to yellow indicates the elapsed time since 12:00 UT. (h) Instantaneous period extracted from mode 6 as a function of the mean magnetic field. The color scheme is the same as in panel (j). “Inst.” means instantaneous, and “a.u.” stands for arbitrary units.
Paper: A 50 minute Coronal Kink Oscillation and Its Possible Photospheric Counterpart
Authors: Sihui Zhong, Valery M. Nakariakov, Dmitrii Y. Kolotkov
Figure caption: The Doppler velocity in the photosphere and chromosphere, and average power spectra from HMI data and CHASE Doppler shift. The CHASE Doppler velocity is derived from the Hα Dopplergram after subtracting the large-scale Doppler velocity including differential rotation. (a) CHASE Hα 6562.82 Å image of ROI. The white box marks ROI1. (b)–(c) HMI Dopplergrams in ROI1, overplotted with contours of −250 G in HMI BLoS at the corresponding time. (d)–(e) Hα 6562.82 Å image (d) and corresponding Doppler velocity map (e) in ROI1. The magnetic pore is outlined by the blue and black −250 G contours of HMI BLoS. (f) Time series of average Doppler velocity in ROI1, with black for Hα LoS velocity, red for HMI Dopplergrams, and blue for HMI Dopplergrams within the magnetic pore (outlined by the blue contour in panel (b)). The dotted sine curve illustrates a 50 minute periodicity for comparison. (g)–(h) Average power spectrum of HMI BLoS (12:00–17:00 UT), HMI continuum intensity (Ic, 12:00–17:00 UT), HMI Dopplergrams (Vlos, 12:00–17:00 UT), and CHASE Hα Doppler velocity (12:00–12:20 UT) in ROI (g) and ROI1 (h). The red curve in panel (h) shows the power spectrum of average HMI BLoS in ROI1 from 12:45 to 17:00 UT (see the black curve in Figure 4(c)). The dotted and dashed lines mark the 5 and 50 minute timescales, respectively. Here, input signals are normalized by their standard deviation to facilitate comparison across different proxies.
Paper: A 50 minute Coronal Kink Oscillation and Its Possible Photospheric Counterpart
Authors: Sihui Zhong, Valery M. Nakariakov, Dmitrii Y. Kolotkov
Figure caption: The spatial location of the 50 minute oscillation of the mean magnetic field in the study region. (a) HMI LoS magnetogram overlaid with two boxes outlining the areas exhibiting 50 minute periodicity. The yellow spline depicts the oscillating loop. The filled area (labeled ROI1) covers the footpoint area of the loop. (b) The detrended mean BLoS in area ROI2 (black). The red curve is the sixth EMD mode with a periodicity of 50.6  ±  5.8 minutes. (c) The detected 50 minute oscillations of average magnetic field strength in areas ROI1–ROI2.
Paper: A Correlation between Fast Radio Burst Dispersion Measure and Foreground Large-scale Structure
Authors: Maryam Hussaini, Liam Connor, Ralf M. Konietzka, Vikram Ravi, Jakob Faber, Kritti Sharma, Myles Sherman
Figure caption: A 2D histogram showing the galaxy number density in the WISE-PS1-STRM for galaxies between 0.10 < z < 0.20. The circles mark our FRB sample colored by redshift.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Volume-integrated cooling rate, Lcool (top panel), and accretion rate, ﹩\dot{M}﹩ (second panel), vs. time for our three binary simulations compared with the single black hole simulation (cyan dashed–dotted line). The vertical purple dotted lines represent the z = 0 crossing times of the q = 0.1 orbit (the q = 0.05 and q = 0.025 crossing times are not shown for visual clarity). The four pairs of panels at the bottom of the figure show zoomed-in views of four disk impact events. Here Lcool is effectively a measure of the instantaneous total heating rate. Each impact of the secondary with the disk results in a spike in Lcool, with broader peaks generally associated with impacts at larger distances from the primary. Typically the peaks in Lcool are followed by broader peaks in the accretion rate 100M–200M later associated with shocked gas that has lost angular momentum.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Volume rendering of our q = 0.1 simulation at four different times, with the top left panel representing the time when the secondary black hole is introduced. Disk colors show temperature (dark purple to white, logarithmic), while green marks magnetized outflow with σ = 1. The yellow lines mark the recent and future orbit for the secondary at each time (moving in the clockwise direction), and the two black spheres represent the primary and secondary black holes. Impacts from the secondary create hot bubbles of gas on both sides of the disk while also heating up the main body of the disk and generating spiral shock waves. Occasionally (twice in the whole simulation), a small jet is produced by the secondary (bottom right panel). Animated version: https://youtube.com/shorts/8pcuUNnYjNQ.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Integrated quantities in our single black hole H/r = 0.1 disk simulation vs. radius and time. Top: time-averaged (40,000M–70,000M) accretion rate, ﹩\dot{M}﹩ (solid blue), and the scale height normalized to the target scale height, H/Htarget (dashed orange), vs. radius. Middle: MRI quality factors defined around Equation (A2), Q(i), vs. radius at t = 70,000M (solid) and t = 83,000M (dashed). Bottom: accretion rate (solid blue), ﹩\dot{M}﹩, dimensionless magnetic flux threading the event horizon (dashed green), ϕBH, and volume-integrated cooling rate (dashed silver), lcool, vs. time. The simulation reaches inflow equilibrium out to ∼25rg (as evidenced by the flat accretion rate profile vs. radius), and the cooling function keeps the scale height close to the target except for inside the ISCO radius and at large distances. The MRI is well resolved in all directions until the quality factors drop after ∼70,000M, at which point the accretion rate also drops by a factor of ∼2. ϕBH saturates around ∼40, and its variability is almost entirely driven by variability in ﹩\dot{M}﹩.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Effects of the secondary on the primary accretion disk for q = 0.1 shown in the midplane pressure (top panel) and a poloidal slice of mass density with magnetic field lines overplotted (bottom panel). The first column is right after the secondary has been added to the simulation, the second column is just after the first impact of the secondary, and the third column is later in the simulation after ∼15 impacts. Each impact produces a spiral shock wave that temporarily boosts the accretion rate (compare with the bottom panel of Figure 4). The repeated interaction with the gravity of the secondary also torques the disk in nontrivial ways, resulting in tilts in both the y–z plane and x–z plane. Animations of this figure are available for the q = 0.1 (https://youtu.be/v1-WId2JKbc), q = 0.05 (https://youtu.be/3aIjSRte-eM), and q = 0.025 (https://youtu.be/6qrMa5xgzpg) simulations.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Angular momentum direction vs. time at r = 7rg in our simulations. Top: angle-averaged x, y, and z components of angular momentum, Li, relative to the total angular momentum, ltot, in our q = 0.1 simulation. Bottom: tilt angle, ﹩{\theta }_{{\rm{tilt}}}=\arccos (\langle {L}_{z}\rangle /\langle {L}_{{\rm{tot}}}\rangle )﹩, in our q = 0.1 (solid purple), q = 0.05 (dotted green), and q = 0.025 (dotted black) simulations. Gravitational torque from the secondary black hole can cause significant tilting of the disk (10°–20° for q = 0.1, 5°–10° for q = 0.05, and a few degrees for q = 0.0025) in both the x- and y-directions (note that the secondary’s orbit is in the y–z plane). This tilt, however, does not strictly increase with time but seems to vary around a saturated value. Spikes in the tilt angle are seen during increased accretion events associated with lower angular momentum spiral streams caused by the secondary’s impacts with the primary accretion disk (see Figures 4 and 5).
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Time series of the first impact of the secondary with the primary’s accretion disk. The color map highlights regions with high ρT1.5, which is a proxy for regions of high emission with our cooling function (Equation (2)). The different rows represent q = 0.1 (top), q = 0.005 (middle), and q = 0.0025 (bottom). All three simulations generally show the same behavior, with a shock cone developing around the secondary as it passes through the disk, resulting in two hot gas bubbles expanding on either side. The sizes of these features decrease with decreasing q.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Poloidal slice of density ρ (left) and plasma β (right) with magnetic field lines overplotted at t = 50,000M from our single black hole, thin-disk simulation. The disk is MRI turbulent with β ≳ 100, surrounded by a lower-density, highly magnetized corona with β ∼ 0.1. Coherent vertical magnetic field populates the inner 10rg–15rg and partially truncates the disk.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Poloidal slice of density ρ (left) and plasma β (right) with magnetic field lines overplotted at t = 70,000M from our single black hole, thin-disk simulation that was restarted from the H/r = 0.1 simulation to have a new H/r = 0.03 target. The much thinner disk is now highly magnetized owing to compression of the magnetic field, with a lower density and faster inflow velocity.