adsabs/AstroCLIMB huggingface dataset:
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Time-averaged profiles of accretion rate ﹩\dot{M}﹩, feedback efficiency η, and shell-averaged angular velocity 〈Ω〉 of torus simulations for different resolutions and BH spins. The runs with lower resolutions (dashed lines) show similar radial profiles as the higher-resolution runs (solid lines) for three different spins (distinguished by different colors).
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: A 2D schematic of the magnetic boundary conditions (bflux0 and bflux-const) similar to H. Cho et al. (2024) but for face-centered magnetic fields.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Cell indices of the first physical layer neighboring the ghost cells when the highest level of de-refinement is n = 1.
Paper: Bridging Scales in Black Hole Accretion and Feedback: Relativistic Jet Linking the Horizon to the Host Galaxy
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Ramesh Narayan, Kung-Yi Su, Priyamvada Natarajan
Figure caption: Comparison of the EKS and JKS coordinate systems. While the θ − grid is uniform at all radius for EKS, θ − grid collimates near the poles at large radius for JKS.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Sandwich corona. The change of the disk fraction (the left panel) and Γ (the right panel) with optical depth (τ = neσTh, where ﹩h={h}_{{\rm{\max }}}-{h}_{{\rm{\min }}}﹩ is the thickness of the corona) and outer corona radius (Rout), observed at i = 60°. We produce the simulation over a 6 × 5 grid (τ = 0.1, 0.3, 0.5, 0.7, 0.9 while Rout = 10, 14, 18, 22, 26, 30 Rg) and perform a 2D interpolation to get the continuous trend and draw the contour lines. The upper triangle and lower triangle show the selected soft-state and hard-state spectra of the sandwich corona in Figure 12. Throughout the paper, the color bars of all the contour plots are the same.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Spherical corona. The change of the disk fraction (the left panel) and Γ (the right panel) with optical depth (τ = neσTR) and corona radius (R), observed at i = 60°. We produce the simulations over a 5 × 5 grid (τ = 1.0, 1.5, 2.0, 2.5, 3.0, while R = 6, 12, 18, 24, 30 Rg) and perform a 2D interpolation to get the continuous trend and draw the contour lines. The upper triangle and lower triangle show the selected soft-state and hard-state spectra of the spherical corona in Figure 12.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Sandwich corona with the black hole spin a* = 0.5 (the upper panels) and a* = 0 (the lower panels). The change of the disk fraction (the left panels) and the photon index (the right panels) with the optical depth and outer radius, observed at i = 60°. The simulation grid is the same as that in Figure 3. The shadowed region indicates the spectra cannot be fit well with χ2/d. o. f. > 2.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Lamppost corona. The change of the disk fraction (the left panel) and Γ (the right panel) with optical depth (τ = neσTR, where R = 2 Rg) and corona height (h) above the disk, observed at i = 60°. We do the simulation on a 5 × 5 grid (τ = 1, 2, 3, 4, 5, while h = 1, 2, 3, 4, 5 Rg) and do a 2D interpolation to get the continuous trend and draw the contour lines. The shadowed region indicates the spectra with σΓ larger than 0.2.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: The change of Γ with corona optical depth given by fitting the compTT model and MONK simulation spectra with simplcut∗diskbb. The left panel shows the result for a disk-like (sandwich) corona, and the right panel shows the result for a spherical corona. Results of different sandwich corona outer radii and spherical corona radii are shown in different colors. While the plots show the general consistency of the changing trend of Γ given by MONK and compTT, the absolute values of Γ show discrepancies depending on the size of the corona.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: The HID of the simulated points of the sandwich corona (left panel) and spherical corona (right panel). The x-axis is the hardness ratio of the count rate of photons between 4 and 20 keV to 2–4 keV, and the y-axis is that of photons between 2 and 20 keV. The size of the point shows the size of the coronas (rescaled), and the color reflects the optical depth. The crosses note the points identified as the soft state in Section 3, while the plus signs note the hard-state points.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: The data, best-fit model, and residuals of the fit of the simulated disk emission of a 10M⊙, a* = 0.998 black hole accreting at 10% of the Eddington mass accretion rate, observed from 10 kpc and 60°. The model kerrbb can fit well the simulated spectrum, with χ2/d.o.f. = 135.23/124 = 1.09.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: The coronal geometries considered in our study. The upper-left panel is the sandwich corona, which is two parallel layers with a certain thickness above and below the disk. The upper-right panel is the spherical corona, which is a central sphere around the black hole. The lower panel is the lamppost corona, which is a sphere of finite radius (=2 Rg in our simulations) along the black hole spin axis.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Sandwich corona with different disk inclinations. The change of the photon index (the upper panels) and disk fraction (the lower panels) with the optical depth and outer radius, observed at i = 40° (the left panels) and i = 80° (the right panels). The simulation grid is the same as that in Figure 3.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Mean-velocity maps of the synthetic C18O emission (first row); expected Keplerian velocity fields after projection onto the plane of the sky (second row); residual velocity maps of the raw simulation data, which are computed using the true gas velocity from the simulations (third row); and residual velocity maps of the synthetic C18O emission (fourth row). From left to right, maps for the MRI, clump-infall, and intruder models are presented. We note that color scales of the residual maps are different for all models. The boundaries between the disks and envelopes, which are defined by a density threshold of 0.1 g cm−2, are denoted by contours. The envelope regions are masked in the residual maps for better visualizations. The dotted curves indicate the locations of the high-density spiral arms. Black crosses indicate the protostellar positions, and green crosses denote positions of an inner clump or the intruder. Contours in the zoom-in view of the residual maps for the MRI model denote zero residual velocities.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Simulated spatial distributions of gas surface density (top row), gas temperature (middle row), and gas scale heights (bottom row) at the time of burst onset for the MRI-triggered burst (left), clump infall (center), and close stellar flyby (right). The arrows point to the infalling clump causing the burst and the intruder.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Left panels: the selected hard spectra of the sandwich and spherical coronas corresponding to the lower triangles in Figures 3 and 4. Right panels: the selected soft spectra of the sandwich and spherical coronas corresponding to the upper triangles in Figures 3 and 4. The upper panels show the simulated 30 ks NuSTAR observations of the energy spectra with the error bars showing the simulated data and the solid lines showing the best-fit simplcut∗kerrbb model. The middle and lower panels show the simulated 100 ks IXPE observations of the PD and PA spectra. The dashed lines in the middle panels present the MDP99 in different energy bins. See the text for more details of the simulation settings.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Surface density (color) and velocity field (vectors) in the MRI model (left), clump-infall model (middle), and close stellar flyby model (right). The Keplerian rotation is subtracted from the model velocity. Note the different spatial scales to better resolve the spatial morphology and velocity fields of the disk. The disk rotates counterclockwise.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Integrated intensity maps of the synthetic C18O J = 3–2 emission for the three models without (top row) and with (bottom row) beam convolution. From left to right, maps for the MRI, clump-infall, and intruder models are presented. The dotted curves indicate the locations of the high-density spiral arms in the first two models. The crosses mark positions of the central protostars and the intruder. In the bottom row, contour levels are 3σ, 6σ, 12σ, and 24σ, where σ = 2.0, 2.2, and 2.6 mJy beam−1 for the MRI, clump-infall, and intruder models, respectively. The filled circle in the bottom left panel denotes the beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }1﹩.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Mass accretion rates and total luminosities in the three burst models considered. The panels from top to bottom correspond to the MRI-triggered burst, clump accretion, and close flyby. The black circles indicate the exact times during the bursts considered in this work.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Four example spectra that cannot be fit well by the simplcut∗kerrbb model. They are the spectra of a a* = 0.5 or a* = 0 black hole with a sandwich corona, with inner radius equaling the ISCO and different outer radii and optical depths noted in the labels. The free parameters in these fits are the mass accretion rate, scattering fraction, and Γ.
Paper: Possible Coronal Geometry in the Hard and Soft States of Black Hole X-Ray Binaries from MONK Simulations
Authors: Ningyue Fan, Cosimo Bambi, James F. Steiner, Wenda Zhang
Figure caption: Change of the disk fraction (left panel) and photon index Γ (right panel) with the optical depth τ for an Rout = 30 Rg sandwich corona with a different temperature around an a* = 0.998 black hole. The disk fraction values for T = 300 keV and τ = 0.7, 0.9 are a bit higher than expected because for these points, the fitting values of Γ hit the lower boundary 1.1, and the fits are not so good.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Velocity channel maps of the synthetic C18O J  = 3–2 emission of the three models without beam convolution. The channel maps are presented in steps of 0.48 km s−1, while the original velocity resolution of the synthetic data is 0.16 km s−1. Green colors and black contours show the synthetic C18O emission. Contour levels are 3%, 10%, 30%, 60%, and 90% of the maximum intensity. The background images in orange show the surface density distributions of the input models. We note that the extent of the channel maps for the clump-infall model is larger than that for the other two models. The dotted curves highlight the locations of the high-density spiral arms.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Residual velocity maps of the beam-convolved C18O J = 3–2 emission, calculated using Keplerian velocity fields with stellar masses smaller (top) and larger (bottom) than the true values by 20%. The dotted curves indicate the locations of the high-density spiral arms. The filled circle in the bottom left panel shows the beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }1﹩. Black crosses indicate the protostellar positions, and green crosses denote positions of the inner clump or intruder.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: The model surface density distributions (top) and residual velocity maps (bottom) for the modified MRI model rotated by an angle of ϕ in the counterclockwise direction. We note that rotation by the inclination angle is not included in the surface density plots. The dotted curves and filled circles in the residual maps denote the locations of the high-density spiral arms and the beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }1﹩, respectively.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Velocity channel maps of the C18O J  = 3–2 emission after beam convolution (green) overlaid with Keplerian isovelocity curves (orange) expected for the protostellar mass. The channel maps are presented in steps of 0.48 km s−1, while the original velocity resolution of the synthetic data is 0.16 km s−1. Contour levels are 3σ, 6σ, 9σ, 12σ, 15σ, and 20σ, where σ = 2.5 mJy beam−1. Dotted curves denote the locations of the spiral arms, and crosses indicate stellar positions. Filled circles in the bottom left corners show the beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }1﹩.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Maps of mean velocity (top row) and residual velocity (bottom row) of the C18O J = 3–2 emission after beam convolution. The dotted curves indicate the locations of the high-density spiral arms. The filled circle in the bottom left panel shows the beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }1﹩. Black crosses indicate the protostellar positions, and green crosses denote positions of an inner clump or the intruder.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: (a) Same as the zoom-in view of the residual map of the MRI model in Figure 5 but with markers that denote the positions where the spectra shown in the right panels were measured. (b), (c) Spectra of the synthetic C18O emission of the MRI model, measured at the positions of the northern inner and outer spirals around the disk minor axis. Vertical solid and dashed lines indicate intensity-weighted mean velocity calculated with the spectra and the true gas velocity at the positions in the numerical simulation, respectively.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Same as the third and fourth rows of Figure 5 but for a geometrically thin MRI model.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Gas surface density (top row) and temperature (bottom row) just before the burst (left column) and during the burst (right column), i.e., 30 yr after the burst onset in the MRI model.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Same as Figure 13 but for the clump-infall model.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Residual velocity maps of the beam-convolved C18O J = 3–2 emission of the modified MRI, clump-infall, and intruder models with inclination angles of 45∘ (top) and 60∘ (bottom). The dotted curves indicate the locations of the high-density spiral arms. The filled circle in the bottom left panel shows the beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }1﹩. Black crosses indicate the protostellar positions, and green crosses denote positions of the inner clump or intruder.
Paper: Morphological and Kinematic Diagnostic of FU Orionis-type Outburst Mechanisms
Authors: Jinshi Sai, Eduard I. Vorobyov, Alexandr Skliarevskii, Michihiro Takami
Figure caption: Same as Figure 13 but for the intruder model.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. IV. Broad Emission-line Evolution Sequence among Hα, Mg II, and Hβ
Authors: Wei-Jian Guo, Victoria A. Fawcett, Małgorzata Siudek, Yan-Rong Li, Cheng Cheng, Swayamtrupta Panda, Zhiwei Pan, Shengxiu Sun, Claire L. Greenwell, David M. Alexander, John Moustakas, Shuo Zhai, Jun-Jie Jin, Huaqing Cheng, Jingwei Hu, Yong-Jie Chen, Zhi-Xiang Zhang, Jian-Min Wang
Figure caption: Optical spectra of the CL-AGN core sample (top panel) and 10 stacked spectra (bottom panel) in the redshift range 0.35 < z < 0.45, color-coded by continuum luminosity at 5100 Å (L5100). The top panel shows individual spectra normalized at 6000 Å to highlight relative emission-line strengths, while the bottom panel displays the corresponding stacked (mean-combined) spectra in luminosity bins. Prominent broad and narrow emission lines, including Mg II, Hβ, and Hα, are visible.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. IV. Broad Emission-line Evolution Sequence among Hα, Mg II, and Hβ
Authors: Wei-Jian Guo, Victoria A. Fawcett, Małgorzata Siudek, Yan-Rong Li, Cheng Cheng, Swayamtrupta Panda, Zhiwei Pan, Shengxiu Sun, Claire L. Greenwell, David M. Alexander, John Moustakas, Shuo Zhai, Jun-Jie Jin, Huaqing Cheng, Jingwei Hu, Yong-Jie Chen, Zhi-Xiang Zhang, Jian-Min Wang
Figure caption: Composite spectra of control sample (Type 1 AGNs) in four black hole mass (MBH) bins, further subdivided by eight Hα luminosity or continuum luminosity at 5100 Å (L5100). The leftmost panels show the full spectral range, while the right panels highlight the emission-line regions of Mg II, Hβ, and Hα. Each stacked curve corresponds to a median spectrum in a specific Hα bin, as labeled. The color coding follows a gradient palette to ensure clear visual differentiation between luminosity bins.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. IV. Broad Emission-line Evolution Sequence among Hα, Mg II, and Hβ
Authors: Wei-Jian Guo, Victoria A. Fawcett, Małgorzata Siudek, Yan-Rong Li, Cheng Cheng, Swayamtrupta Panda, Zhiwei Pan, Shengxiu Sun, Claire L. Greenwell, David M. Alexander, John Moustakas, Shuo Zhai, Jun-Jie Jin, Huaqing Cheng, Jingwei Hu, Yong-Jie Chen, Zhi-Xiang Zhang, Jian-Min Wang
Figure caption: Optical spectra of the CL-AGN core sample (top panel) and 10 stacked spectra (bottom panel) in the redshift range 0.35 < z < 0.45; same as Figure 1 but color-coded by Eddington ratio (λEdd).
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: 2023 Reverberation Mapping Results
Authors: Wen-Zhe Xi, Kai-Xing Lu, Jin-Ming Bai, Zhang Yue, Weimin Yi, Liang Xu, Sha-Sha Li, Hai-Cheng Feng, Jian-Guo Wang
Figure caption: Light curves and the results of cross-correlation analysis. The left panels ((a)–(e)) are the light curves of the AGN continuum at 5100 Å and the broad He II, He I, Hγ, and Hβ emission lines; the contamination of this data by the host galaxy has been eliminated by spectral decomposition. The red arrows indicate a transient dip in the AGN continuum and the corresponding time-delayed dip in the emission line flux. The horizontal dotted lines represent the mean flux. The right panels ((aa)–(ea)) are corresponding to the ACF of the continuum and the CCF between the broad-line light curves (b)–(e) and the continuum variation (a); the histogram in black is the cross-correlation centroid distribution (CCCD). We note the variability amplitude of Fvar in panels (a)–(e) and the maximum cross-correlation coefficient of ﹩{r}_{{\rm{\max }}}﹩ in CCF panels (ba)–(ea). The measured time lags in the rest frame are marked by the vertical dashed lines in panels (ba)–(ea); the vertical dotted lines are reference lines of zero time lag. The units of F5100 and emission lines are ﹩{\rm{erg}}\,{{\rm{s}}}^{-1}\,{{\rm{cm}}{}^{-2}\,\mathring{\rm A} }^{-1}﹩ and erg s−1 cm−2, respectively.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: 2023 Reverberation Mapping Results
Authors: Wen-Zhe Xi, Kai-Xing Lu, Jin-Ming Bai, Zhang Yue, Weimin Yi, Liang Xu, Sha-Sha Li, Hai-Cheng Feng, Jian-Guo Wang
Figure caption: Spectral fitting and decomposition of the mean spectrum calculated from the calibrated spectra. Panel (a) illustrates the details of spectral fitting and decomposition, where the mean spectrum is shown in lime; the total model in red; and the fitting components include the AGN continuum (blue), iron multiplets (navy), host galaxy (gray), broad Balmer lines (solid magenta), narrow Balmer lines (dashed magenta), broad helium lines (cyan), narrow helium lines (orange), [O III] narrow lines (dashed orange), and other weak narrow emission lines (solid orange). Vertical reference lines are added at the rest wavelengths to mark the broad Hγ, He II, Hβ, He II, and [O III] λ5007 lines. Panel (b) displays the fitting residuals in percentage. Panel (c) presents the net broad Hγ, He II, Hβ, and He I lines, where the fitted broad-line profiles (models) are indicated by red dashed lines, and the broad-line profiles after subtracting other fitted components from the spectrum are shown in black.