adsabs/AstroCLIMB huggingface dataset:
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Magnetic modeling and width measurements of the representative late-phase loop. Panel (a) shows an AIA 171 Å image of the late-phase region, with the dotted line tracing the representative late-phase loop. A zoomed-in view of the region enclosed by the dashed box is displayed in panel (b), where we put a total of eight slices (numbered from 1 to 8 toward the close-to-apex box) locally perpendicular to the loop spine for width measurement. Panel (c) overlays some magnetic field lines traced from the NLFFF extrapolation, and panel (d) plots the variations of the magnetic strength and height along a proxy field line (the red line in panel (c)) that best matches the representative late-phase loop. The dashed–dotted box in panel (d) represents the extent of the loop segment used for width measurement. Panels (e) and (f) demonstrate the results of Gaussian fitting (the dashed–dotted lines) to the AIA intensities (asterisks) along slices 1 and 8, respectively, with the fitted loop widths labeled in the legend as well, and panel (g) shows the tendency of the loop width variation based on the fitting results for all slices. Note that the error bars are estimated from the fitting uncertainties.
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Eruption process of the filament-hosting MFR. Panels (a) and (b) show snapshots of the MFR eruption in AIA 131 and 304 Å, respectively. Panels (c) and (d) display the time–distance stack plots of the AIA 131 and 304 Å intensities along the slice (dashed–dotted line) drawn in panels (a) and (b). A zoomed-in view of the part bounded by the dotted lines in panel (d) is also displayed in panel (e), in which the position of the MFR apex is traced by the plus signs. Panel (f) plots the variation of the MFR velocity (in blue) according to the time–distance measurements shown in panel (e), as well as the RHESSI 50–100 keV count rate for this flare (in orange). The vertical dashed–dotted–dotted lines mark the peak times of the two profiles.
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Time profiles of the GOES 1–8 Å SXR flux (a) and the background-subtracted EVE full-disk irradiance (black) and AIA subregion intensities (colored) in several lines and passbands (b)–(d) for the 2012 October 23 X1.8 flare. The vertical dashed–dotted–dotted lines mark conspicuous peaks of the GOES flux and AIA intensities, and the horizontal dashed lines in panels (b)–(d) denote the background levels for EVE and AIA data. Note that a 100–150 s smoothing boxcar is applied to the EVE raw data points (dot signs), and the AIA subregion covers a field of view of 210″ × 210″ enclosing the flare-hosting AR.
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Evolution of the representative late-phase loop. Left: snapshots of the AIA 131 Å images showing the late-phase region, where the representative late-phase loop is traced by the dotted line and overlaid by a 5″ × 5″ box near its apex. Right: thermodynamic evolution for the selected box. Panel (c) plots the AIA 131Å, 335Å, and 171 Å light curves over the box, where the vertical dashed–dotted–dotted lines represent the peak times in AIA 131Å and 171 Å, respectively. Panels (d) and (e) depict the corresponding DEM distributions (plus the results of 100 Monte Carlo simulations, in blue) at these two peak times. For comparison, the pre-event DEM for the box (in gray) is also overplotted.
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: DEM inversion results for the flare. Left: EM maps of the AR at two moments when the main-phase (enclosed by the blue contour in panel (a)) and late-phase (enclosed by the orange contour in panel (b)) regions are well developed, respectively. Right: temporal evolutions of the volume EM (c) and DEM-weighted temperature (d) for the two regions (discriminated by the colors). The vertical dashed–dotted–dotted lines in panel (c) indicate the times of maximum volume EM for the main-phase and late-phase regions, respectively.
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Variation of the eigenvalue k (a) and conductive cooling time τ  c  (b) vs. the expansion factor Γ according to the semi-analytical solution for conductive cooling (Equations (B17) and (B18)).
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Synthetic and observed EVE light curves in several lines (discriminated by the colors). The synthetic curves are derived from the AIA-based DEM inversion results for the flaring region, and the observed curves are displayed in the same way as in Figure 1. In each panel, the cross-correlation coefficient between the two curves is calculated and labeled in the legend. All the time profiles are plotted with the corresponding background levels subtracted.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Morphology of the core of NGC 5084 obtained with Hubble. Left: LRGB image generated using four HST filters: WFC3/UVIS F475W (blue), WFPC2 F658N (green), WFPC2 F702W (yellow), and WFC3/IR F160W (red). The area shown is 12.6 × 12.6 arcsec2 (1.82 × 1.82 kpc2 at a distance of 29.91 Mpc). Right: analysis of the ellipticity of the circumnuclear disk of NGC 5084. Yellow ellipses show the bootstrapping + Monte Carlo elliptical fits, displaced 1″ (the double-headed arrow shows the offset distance) to the west from the core of the galaxy to enhance the visual comparison. The results of the fit are shown in the panel. The black crosses show the best fit to the center of the fitted ellipses. HST/WFPC2 F702W flux is shown in the background. Note that the RGB color levels in the left panel have been optimized to emphasize the disk. Photometric color maps (g − r and F475W–F702W) are available in Figure 10. See the scale and color bars for reference.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Comparison of EVLA radio-wavelength 6 cm observations with the optical and X-ray morphology of NGC 5084. Blue contours represent the 3σ, 5σ, and 10σ confidence levels at 6 cm in EVLA Band C observations from CHANG-ES (T. Wiegert et al. 2015). The sensitivity for VLA C-band observations is 7.9 μJy beam−1 in 15.64 × 8.35 arcsec−2. In the background, the optical gri RGB image of NGC 5084 from the Pan-STARRS image (K. C. Chambers et al. 2016). White contours represent the emission in the Chandra/ACIS X-ray soft band (0.3–2.0 keV) in s−1 cm−2 arcsec−2.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Velocity field analysis of the circumnuclear disk of NGC 5084, based on ALMA CO(2–1) observations. Left: spectral analysis of the redshifted (z = 0.005741) CO(2–1) emission line ﹩{\nu }_{\mathrm{rest}}^{\mathrm{CO}(2-1)}=230.538\,\mathrm{GHz}﹩. The blue line shows the integrated spectra as a function of the frequency (top axis) and the rotation velocity (bottom). The horizontal dashed line and red dots represent the line width at half-maximum. The vertical dashed line represents the center of the redshifted CO(2–1) emission line. Right: CO(2–1) velocity map (see the right color bar) over the WFPC2/F702W intensity map (bottom color bar). The yellow ellipse represents ALMA observations beam size ([B maj, B min]=[0.60, 0.54] arcsec).
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Diffuse X-ray emission of NGC 5084 as detected with SAUNAS/Chandra in the 0.3–2.0 keV broadband. Left: X-ray contours (this work) overplotted on the optical gri color Pan-STARRS image (K. C. Chambers et al. 2016). Right: SAUNAS map of the diffuse X-ray emission, corrected for PSF, point sources, and sky background. Solid, dashed, and dotted contours represent the 5σ, 3σ, and 2σ detection levels of X-ray emission, represented in white (left panel) and black (right panel) for contrast.
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Temporal evolutions of the looptop temperature (a), pressure (b), density (c), and mass flow through the loop base (d), based on the analytical solutions for radiative cooling (Equations (B47)–(B49) and (B51)). The curves are calculated with commonly adopted values of γ and l at 5/3 and 1/2, respectively. The different line styles denote cases of different values of α in the T–n scaling relation (indicated in the legend).
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Regions assigned for spectral analysis. Left panel: white contours in the left panel represent the 2σ, 3σ, 5σ, 7σ, and 10σ detection limits in the 0.3–2.0 keV band from Chandra/ACIS. The slit-shaped regions (1.″5 wide) represent the APO/DIS optical spectra, defined to align with the major axis of the galaxy and the major axis of the circumnuclear disk. The circular core region, shown in the zoomed image, has a 3″ radius. The RGB background image was generated using the gri observations from Pan-STARRS. Right: close-up view of the core regions, showing the apertures for optical 6dF spectra (R = 3.″4), and the APO/DIS slit spectra. The background image represents the flux intensity in the F475W band from HST/WFPC2.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Morphological structure of NGC 5084 in X-ray, optical, and NIR wavelengths. Left panel: optical and X-ray image of the disk of NGC 5084. Background: luminance-red, green, and blue (RGB) image (Telescope: CDK17. Camera: SBIG STXL-11002M. Filter: Astrodon Gen 1 LRGB E-Series. Credit: Martin Pugh and Brian Diaz). FOV: 15 × 15 arcmin2. Right panel: high-resolution luminance-RGB image zoom of the core of NGC 5084 based on HST observations. Blue: WFC3/UVIS F475W. Green: WFPC2 F658N. Yellow: WFPC2 F702W. Red: WFC3/IR F160W. FOV: 24 × 24 arcsec2. See the legend for the color-band description and the physical scale bars in the panels for reference.
Paper: Enhanced Peak and Extended Cooling of the Extreme-ultraviolet Late Phase in a Confined Solar Flare
Authors: Shihan Li, Yu Dai, Mingde Ding, Zhen Li, Jinhan Guo, Hao Wu
Figure caption: Profiles of the loop temperature (a), cross-sectional area (b), heat flux (c), and total conductive losses (d) based on the semi-analytical solutions for conductive cooling. The curves are calculated with different values of the expansion factor (discriminated by different line styles).
Paper: Extreme-mass-ratio Inspirals in the Strong Segregation Regime—to Inspiral or to Get Ejected?
Authors: Karamveer Kaur, Hagai B. Perets
Figure caption: Evaluation of the critical semimajor axis a c0. Here, we show the streamlines (in blue) in the ﹩\{a,{ \mathcal R }\}﹩ plane indicating the net flow of BHs at the end of simulations (t = T 2b(a c)) without strong scatterings. Different panels correspond to γ = {2, 2.25, 2.5} while fixing M • = 106  M ⊙. Evidently, the analytical estimate a c (dotted magenta line) of the critical semimajor axis (Equation (4)) is not completely accurate and streamlines initiating at a ∈ (a c0, a c) end up in plunging orbits inside the capture radius (solid gray line). Hence, a c0 ≪ a c is a better estimate of the critical semimajor axis, as most streamlines inside with initial a ≤ a c0 lead to inspiral orbits that eventually evolve into EMRIs. As γ increases to the right, a c0/a f becomes smaller (and its departure from a c/a f is greater) due to a narrowing GW loss cone (the region enclosed between the dashed and solid gray lines, given by 4R  s  ≤ r  p  ≤ r  p,gw). However, a c0/a f is almost independent of M •, with a c0/a f = {0.094, 0.032, 0.007} for γ = {2, 2.25, 2.5}.
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Results obtained for 3C 391. Top panel: T 97, the temperature derived from the relative populations in the H2 J = 7 and 9 states. Middle panel: OPR789, the ortho-to-para ratio derived from the relative populations in the H2 J = 7, 8, and 9 states. Bottom panels: scaled spectra, rebinned to 2 km s−1 resolution, with the same color coding as in Figures 4–6.
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Results obtained for NGC 2071. Top two panels: T  XY , the temperature derived from the relative populations in the H2 J = X and Y states. Next two panels: OPR XYZ , the ortho-to-para ratio derived from the relative populations in the H2 J = X, Y, and Z states. Bottom panels: scaled spectra, rebinned to 2 km s−1 resolution, with the same color coding as in Figures 4–6.
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Same as Figure 4, but for NGC 2071
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Top: our M BH–M ⋆ relations at different redshifts, plotted as the colored curves. The original TNG-simulated z = 0 relation is shown as the black solid curve for comparison. We also plot the relations in J. Kormendy & L. C. Ho (2013), J. I. H. Li et al. (2023), J. E. Greene et al. (2020), A. E. Reines & M. Volonteri (2015), F. Shankar et al. (2016), and G. A. D. Savorgnan et al. (2016) as the black dashed lines, which are labeled as KH13, L23, G20, RV15, Sh16, and Sa16, respectively. Two relations in A. E. Reines & M. Volonteri (2015) are included—one based on the SMBH sample with dynamically measured M BH, and the other based on the AGN sample; these two are labeled as RV15-dyn and RV15-AGN, respectively. The highest three relations are labeled together as “KH13; RV15-dyn; Sa16” for a better visualization, and they are all from dynamically measured SMBHs in early-type galaxies. Our recovered relations are apparently lower than the original TNG relation and the early-type dynamically measured ones. Middle: our recovered 1σ M BH scatter in dex vs. M ⋆. Bottom: the fractional contribution of SMBH growth along different M ⋆ evolutionary tracks to our recovered variance, which is one minus the fraction of variance from seeding scatter.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Example M ⋆ and M BH evolutionary tracks for MW-like galaxies (left) and massive galaxies with ﹩{M}_{\star }\approx 10{M}_{\star }^{\mathrm{MW}}﹩ (right). Each panel presents one galaxy at z = 0 and all of its progenitors with M ⋆ > 109.5 M ⊙ at previous snapshots. Each black point marks one massive galaxy with M ⋆ > 109.5 M ⊙ at the corresponding snapshot, and dwarf galaxies are not shown for visual clarity. Cyan and blue lines connect galaxies with their descendants in terms of M ⋆ and M BH, respectively. A few cyan lines drop down at ≈109.5 M ⊙ without connecting to descendant points because their descendants have M ⋆ < 109.5 M ⊙ and are thus not shown, but these galaxies will eventually merge to form the final z = 0 galaxy. The massive-galaxy example in the right panel apparently undergoes more mergers with massive galaxies than for the MW-like example in the left panel, which undergoes only one merger with massive galaxies.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Example evolutionary tracks on the M BH–M ⋆ plane. The black star marks the MW. The gray curves represent individual MW-like galaxies. The other three multicolor curves are color-coded by the redshift. The one connected to the black star is the median track of MW-like galaxies, and the other two are the median tracks of galaxies with ﹩{M}_{\star }\approx {M}_{\star }^{\mathrm{MW}}﹩ and ﹩{M}_{\star }\approx 10{M}_{\star }^{\mathrm{MW}}﹩. The dashed line is the AGN-based M BH–M ⋆ relation in A. E. Reines & M. Volonteri (2015).
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Our adopted p merge based on M. Tremmel et al. (2018b) as a function of M ⋆ at different q bins. Term p merge is set to 0 for q < 0.03 and is extrapolated only in the massive end (M ⋆ > 1011.5 M ⊙).
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The BHMF at z = 0. We show M BH ϕ(M BH) instead of ϕ(M BH) to illustrate the typical M BH range where most SMBH mass resides. The blue open circles with 1σ error bars are our BHMFs, where the uncertainties only represent the limited number of sources included in the simulation boxes. The blue dashed line is the resulting BHMF with an additional scatter of 0.5 dex added to our M BH. The black open circles and squares with 1σ error bars are the BHMFs in the original TNG300 and TNG100 simulations. The BHMFs in E. Gallo & A. Sesana (2019), A. Sicilia et al. (2022), and F. Shankar et al. (2020a, 2009) are also plotted, as labeled in the legend. The lighter shaded region shows the uncertainty range in F. Shankar et al. (2020a) considering the uncertainties of scaling relations between M BH and galaxy properties (see also A. Sicilia et al. 2022), and the darker shaded region is the BHMF in F. Shankar et al. (2020a) based on the scaling relation after correcting for the selection bias of dynamically measured SMBHs.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The evolutionary tracks of M BH (top) and M ⋆ (bottom) for the main progenitors’ masses (left) and all the progenitors’ total masses (right), where sources are binned with an M BH(z = 0) width of 0.5 dex. The solid and dashed curves are ﹩\mathrm{log}[\mathrm{median}({M}_{\mathrm{BH}})]﹩ (﹩\mathrm{log}[\mathrm{median}({M}_{\star })]﹩) and ﹩\mathrm{log}[\mathrm{mean}({M}_{\mathrm{BH}})]﹩ (﹩\mathrm{log}[\mathrm{mean}({M}_{\star })]﹩) tracks, respectively. The large points on the curves represent when half of the masses are assembled.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The growth rates as functions of M ⋆ at different redshifts. The red shaded regions represent the 90% confidence range of ﹩{\dot{M}}_{a}﹩ in F. Zou et al. (2024). The blue curves represent ﹩{\dot{M}}_{m}﹩, and the corresponding solid and dashed curves represent the p merge in M. Tremmel et al. (2018b) and p merge = 1, respectively. The cyan curves correspond to TNG100 ﹩{\dot{M}}_{m}﹩ when considering MBHs in dwarf galaxies, where the solid and dashed ones represent our best-guess and extreme, hard-limit cases, respectively.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Same as Figure 10, but for the growth rates as functions of M BH, where we use our M BH–M ⋆ scaling relation to convert M BH to M ⋆. The black vertical lines are the transitioning M BH predicted in F. Pacucci & A. Loeb (2020) when ﹩{\dot{M}}_{a}={\dot{M}}_{m}﹩ at the corresponding redshifts.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption:                       ﹩{\dot{M}}_{a}﹩ vs. M ⋆ at different redshifts. The solid and dashed curves are from the original TNG300 simulation and the observed relation in F. Zou et al. (2024), respectively. There are orders-of-magnitude differences between the simulated and observed ﹩{\dot{M}}_{a}﹩, and the simulated ﹩{\dot{M}}_{a}﹩ often lacks a positive correlation with M ⋆.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Median ﹩{M}_{\mathrm{BH}}({\dot{M}}_{a}=0)/{M}_{\mathrm{BH}}﹩ vs. M ⋆ at different redshifts. The horizontal black dashed line represents ﹩{M}_{\mathrm{BH}}({\dot{M}}_{a}=0)/{M}_{\mathrm{BH}}=0.5﹩.