adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: uGMRT 685 MHz luminosity vs. (top left) molecular gas depletion time, (top right) molecular gas fraction, (middle left) SFE, (middle right) CO(1–0) luminosity, (bottom) SFR, for the uGMRT-observed PG sample. The color bar in all figures, except in the bottom panel, represents the absolute accretion rate. The color bar in the bottom panel represents the CO(1–0) luminosity.
Paper: Internal Activities in a Solar Filament and Heating in Its Threads
Authors: Hengyuan Wei, Zhenghua Huang, Chuan Li, Zhenyong Hou, Ye Qiu, Hui Fu, Xianyong Bai, Lidong Xia
Figure caption: The triggering process of the filament activation in AIA 304 Å from 16:51:29 UT to 16:58:05 UT. (a) The snapshot of AIA 304 Å observation at 16:51:29 UT; the green dashed line marks the position of an arcade overlying the filament, and the cyan dashed line marks a nearby loop. (b) The snapshot of AIA 304 Å observation at 16:52:05 UT; the green and cyan dashed lines mark the arcade and loop after reconnection. (c) The snapshot of AIA 304 Å observation at 16:53:53 UT; the blue arrows point to the eastern filament footpoint, which begins to split. The yellow arrow points to the first localized brightening. (d) The snapshot of AIA 304 Å observation at 16:55:17 UT; the blue arrows point to the eastern filament footpoint, which has split, and the white dashed line marks another brightened arcade. (e) The snapshot of AIA 304 Å observation at 16:56:05 UT; the diamonds in different colors resemble the position of bright points near the eastern footpoint of filament in AIA 94, 131, 171, 193, 211, 304, and 335  Å passbands. (f) The snapshot of AIA 304 Å observation at 16:58:05 UT.
Paper: Internal Activities in a Solar Filament and Heating in Its Threads
Authors: Hengyuan Wei, Zhenghua Huang, Chuan Li, Zhenyong Hou, Ye Qiu, Hui Fu, Xianyong Bai, Lidong Xia
Figure caption: Dopplergrams of the region of interest in the wavelength of H α. (a)–(d) The Dopplergrams in 16:45:04 UT, 16:53:20 UT, 16:54:33 UT, and 16:55:42 UT. The white lines contour the blueshift at the level of 1 km s−1. The black lines in panels (b)–(d) show the contours of redshift at the level of 0.8 km s−1. The red rectangles marked with L1, L2, and L3 show the positions where we obtain the spectral profiles shown in Figure 5. The green contours in panel (d) mark the localized brightenings in AIA 171 Å on 16:55:45 UT at a level of 3000 DN.
Paper: Internal Activities in a Solar Filament and Heating in Its Threads
Authors: Hengyuan Wei, Zhenghua Huang, Chuan Li, Zhenyong Hou, Ye Qiu, Hui Fu, Xianyong Bai, Lidong Xia
Figure caption: Evolution of the spectral profiles at the redshift regions marked as L1, L2, and L3 in Figure 4. The black, blue, cyan, green and red lines in panels (a)–(c) show the spectral profiles at L1, L2, and L3 at 16:45:04 UT, 16:47:27 UT, 16:50:58 UT, 16:54:33 UT, and 16:55:42 UT. The purple dashed line represents the position of line core of reference spectral profile.
Paper: Internal Activities in a Solar Filament and Heating in Its Threads
Authors: Hengyuan Wei, Zhenghua Huang, Chuan Li, Zhenyong Hou, Ye Qiu, Hui Fu, Xianyong Bai, Lidong Xia
Figure caption: Slice–time plot along the red dashed lines in Figures 1(g) and (i). The blue arrows in panels (a) and (b) point to several still, localized brightenings. The green dashed lines in panel (a) trace some moving brightenings.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Plots of the globally measured bar quantities as a function of time. Top: the bar amplitude ( A m=2, scaled m = 2 Fourier amplitude); Bottom: the buckling amplitude ( A buck, scaled m = 2 asymmetry about the midplane). Each color represents a different model grown as a branch from Model C. The curves therefore begin at the time the SMBH is introduced. The SMBH growth period for each model is indicated by the vertical shaded regions of the same color.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Similar to Figure 1. Models ﹩{\widetilde{{BF}}}_{0i},{\widetilde{{BF}}}_{0{ii}}﹩ are analogous to BF 0, and Models ﹩{\widetilde{{AB}}}_{1i},{\widetilde{{AB}}}_{1{ii}}﹩ are analogous to AB 1 but are evolved from the corresponding scrambled initial conditions ﹩{\widetilde{C}}_{i},{\widetilde{C}}_{{ii}}﹩. The vertical orange and purple bands at ∼t = 0 show where the SMBH in the BF 0 analogs grow and the green and brown bands show where the SMBH in the AB 1 analogs grow. Similarly to Figure 1, the early introduction of an SMBH in Models ﹩{\widetilde{{BF}}}_{0i},{\widetilde{{BF}}}_{0{ii}}﹩ does not reduce the bar amplitude in absolute terms.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Similar to Figure 1, to test the impact of stochasticity on the initial conditions of Model C (see the text for details on how initial conditions for ﹩C^{\prime} ﹩, ﹩{\widetilde{C}}_{i}﹩, and ﹩{\widetilde{C}}_{{ii}}﹩ were generated). All models were run under identical parameters to Model C.
Paper: Internal Activities in a Solar Filament and Heating in Its Threads
Authors: Hengyuan Wei, Zhenghua Huang, Chuan Li, Zhenyong Hou, Ye Qiu, Hui Fu, Xianyong Bai, Lidong Xia
Figure caption: A scenario interpreting the reconnection process in this event. (a) The initial magnetic structures. The green and blue lines resemble the magnetic field lines hosting dips and supporting the filament threads, which are shown by orange ovals. The purple lines mark the arcades overlying the filament. The yellow line is the small loop nearby. The red line shows background magnetic field. (b) The time after reconnection between arcade and nearby loop. The gray and cyan lines mark the post-reconnected loop and arcade, respectively. (c) The internal reconnection between different magnetic field lines hosting dips. (d) The time after internal reconnection. The cyan and gold lines mark the post-reconnected arcades. (e) The external reconnection. (f) The time after external reconnection. The brown line marks A2 only observed in AIA 94 Å passband, and the yellow line shows another post-reconnected arcade.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: The values of R pea (top) and h pea (bottom) plotted as a function of the bar amplitude at the final time step. The points with black edges are the control models. Cyan points are Models C, BF 0, BB 1...; red points are Models ﹩\widetilde{{C}_{i}}﹩ and its BF 0, AB 1 analogs; and gray points are ﹩\widetilde{{C}_{{ii}}}﹩ and its BF 0, AB 1 analogs. The gray points overlap significantly since all of these models have nearly identical behavior.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Projected logarithmic surface density maps of selected models at the final snapshot of the simulation (evolution time = 7.568 Gyr). Each projection orientation is normalized by the maximum projected surface density of Model C viewed from that orientation. Therefore, for each orientation all models share a common normalization in which 0 represents the maximum density of Model C in that orientation, and are directly comparable. The increased prominence of the bar and BP/X bulges of models in which an SMBH is grown early (Models BF 0, BB 1) is clearly evident.
Paper: Internal Activities in a Solar Filament and Heating in Its Threads
Authors: Hengyuan Wei, Zhenghua Huang, Chuan Li, Zhenyong Hou, Ye Qiu, Hui Fu, Xianyong Bai, Lidong Xia
Figure caption: Estimation of the width of filament and several localized brightenings. (a) The image observed in AIA 171 Å in 16:58:33 UT. The white line resembles the position where we estimate the width of the filament. The blue, cyan, green, yellow, and red lines resemble the position where we estimate the width of localized brightenings. (b)–(g) The dotted lines show the intensity distributions along the trajectory in panel (a). The black lines show the Gaussian-fit results.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Evolution of velocity dispersion and velocity anistropy as a function of radius in the stellar disk. Each row corresponds to a particular model as labeled. The left column shows radial velocity dispersion (σ  R ), the center column shows vertical velocity dispersion (σ  z ), and the right column shows the ratio (σ  z /σ  R ). In cases where an SMBH is present, a transparent shaded region marks the growth period of the SMBH beginning at its introduction, ending when the SMBH has reached full mass. The time of peak buckling amplitude for each model is indicated by a thin vertical white line. σ  z /σ  R  begins to increase shortly after introduction of the SMBH in Models BF 0 and BB 1 thereby partially stabilizing the disk against buckling, whereas in Model C, σ  z /σ  R  remains effectively constant at all radii until buckling.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Histograms of the logarithm of the spherical pericenter radius in kiloparsecs for Models C, BF 0, and AB 1 at two different times (dashed–dotted lines are for t = 4.54 Gyr, solid lines are for t = 7.57 Gyr). At t = 4.54 Gyr (only 0.75 Gyr after the SMBH has been introduced), Model AB 1 differs only slightly from Model C. All three models have a significant peak at log(r per/kpc) < −1. By the end of the simulation, the peak in Model AB 1 at small r per has decreased. In contrast, Model C shows no significant change in the distribution, while in Model BF 0, the peak has significantly increased despite the presence of the massive black hole. The approximate location of the sphere of influence r BH of the SMBH is shown in BF 0 and AB 1 by the vertical dotted lines, clearly indicating that orbits associated with the central peak in model BF 0 have r per well within the SMBH’s sphere of influence.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Frequency maps in Cartesian coordinates for the same set of 105 orbits at t = 4.54 Gyr and t = 7.57 Gyr for Model C (top row), Model AB 1 (middle row), and Model BF 0 (bottom row). Orbits in each panel are colored by the logarithm of their spherical pericenter radius r per in that snapshot. Several resonances are marked in each panel as (l, n, m) where the integers are coefficients of resonant conditions lΩ x  + mΩ y  + nΩ z  = 0. The orbits clustered around the diagonal resonance line ((1, − 1, 0)) at the bottom-right corner of each panel are primarily associated with the disk rather than the bar (see Valluri et al. 2016, for exceptions).
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Approximate locations of the ILR and vILR in three models (legend) at five times (titles). Horizontal dotted lines show the corresponding bar pattern speeds, with lengths representing bar lengths. Thin solid curves show the rotation frequency Ω(R), thick solid curves show Ω(R) − κ/2, and dashed–dotted curves show Ω(R) − ν(R)/2 (see the text). The bottom-right panel shows the approximate radius of the ILR (thick solid lines) and vILR (dashed–dotted lines) in each model as a function of time. The model with early SMBH introduction, BF 0, develops an ILR and a vILR earlier than the control Model C, and these resonances sweep through the disk to much larger radii (∼4.5–5 kpc, compared to ∼3–3.5 kpc).
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Histograms of frequency ratios for the same particles at different times (rows). The two left columns refer to Model C, and the two right columns refer to model BF 0. The corotation ((Ω ϕ  − Ω P ) = 0), the ILR ((Ω ϕ  − Ω P )/Ω R  = 0.5), and the vILR ((Ω ϕ  − Ω P )/Ω z  = 0.5) are strongly populated.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Mock IFU kinematic data generated from the final snapshot of Model C, BF 0, BB 1, and AB 1 (top to bottom), with the disk face-on and the bar aligned along the x-axis. From left to right: projected surface density and depiction of the kinematic field of view, line-of-sight velocity v, velocity dispersion σ, Gauss–Hermite coefficients h 3 and h 4 (as labeled).
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Number of orbits associated with important resonances seen in Figure 10. Orbits that lie with frequency ratios within 5 × 10−3 of each of these resonance lines are shown at two snapshots as indicated.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Same as Figure 13 with galaxies viewed edge-on and bar viewed side-on.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Similar to Figure 8, but for the Model AB 1 where the SMBH is introduced late, after bar buckling. The ILR and vILR are less populated than in Model C in the final snapshot.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: Results: scatter plots between different physical variables for confined (blue) and eruptive (red) events (>M1.0 GOES flare class). In the corner, we show Spearman correlation coefficient r  s  between each pair of plotted variables for all flares (black) and eruptive (red) and confined (blue) flares separately, where bold and dim fonts indicate the statistical significance of the correlation with p-values below and above p = 0.01, respectively. The values in the parentheses show values for flares above M3.0. See Section 3.2 for details.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: Results: distributions of various physical variables for eruptive (red) and confined (blue) events (>M1.0 GOES flare class). Vertical dotted lines and numbers in the top right corner indicate the mean value for each variable within eruptive and confined flare groups. Darker-color histograms near dotted lines show distributions of the mean, if we select 100 random subsamples of half of the events in each sample, and reflect the variability of the mean due to event selection. See Section 3.1 for details.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: Our SolarErupDB data set of 480 flares (152 eruptive and 328 confined flares), including 103 eruptive and 113 confined M- and X-class flares (see Section 3) and 49 eruptive and 215 confined C-class flares (see the Appendix). Top panel: number of confined and eruptive C-, M-, and X-class flares each month analyzed in this paper (left axis) and sunspot number from 2010 April until 2016 April (right axis). These flares correspond to all events above C5.0 from the flare ribbon database RibbondDB. Bottom panel: flare peak X-ray flux and latitude grouped by AR vs. time; circle size and color correspond to the peak X-ray flux summed over each AR number. See Section 2 for details.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: Distributions of various physical variables for eruptive (red) and confined (blue) events (>C5.0 GOES flare class). Vertical dotted lines and numbers in the top right corner indicate the mean value for each variable within eruptive and confined flare groups. Darker-color histograms show distributions of the mean, if we select 100 random subsamples of half of the events, and reflect variability of the mean due to event selection bias. See the Appendix for details.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: Results: correlation matrix showing Spearman correlation coefficient, r  s , between different physical variables for all flares with GOES flare class >M1.0. We describe the qualitative strength of the correlation using the following guide: r  s  ∈ [0.2, 0.39]—weak, r  s  ∈ [0.4, 0.59]—moderate, r  s  ∈ [0.6, 0.79]—strong, and r  s  ∈ [0.8, 1.0]—very strong. See Section 3.2 for details.
Paper: Early-growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
Authors: Vance Wheeler, Monica Valluri, Leandro Beraldo e Silva, Shashank Dattathri, Victor P. Debattista
Figure caption: Similar to Figure 6 for control model ﹩{\widetilde{C}}_{{ii}}﹩ and its BF 0 and AB 1 analogs.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: X1.2 class eruptive solar flare observed by SDO in the 1600 and 304 Å wavelengths. Bright ribbons mark the footpoints of reconnected field lines that provide an indirect measurement of the amount of reconnecting magnetic flux in the flare and the reconnection rate.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: Results: correlation matrix showing Spearman correlation coefficient between different physical variables for all flares with GOES flare class >C5.0. See the Appendix for details.
Paper: Chemical Evolution of Some Selected Complex Organic Molecules in Low-mass Star-forming Regions
Authors: Bratati Bhat, Rumela Kar, Suman Kumar Mondal, Rana Ghosh, Prasanta Gorai, Takashi Shimonishi, Kei E. I. Tanaka, Kenji Furuya, Ankan Das
Figure caption: The evolution of abundances in different stages of low-mass star-forming regions. The left panel shows the abundances obtained from the RD method (dashed parts are the upper limits), and the right panel depicts the same obtained with the MCMC fitting. Black vertical lines represent the error bars. For CH3OCH3 in L1544 and B1b, the lines have the same upstate energy, so a rotation diagram cannot be performed, and the column density is calculated using simple LTE fitting. For CH3OCH3 in SVS13A, the column density is calculated using the value from Bianchi et al. (2019) scaling it for a 30″ beam. A new class 0 source, IRAS16293-2422 (22 L ⊙), is included where CH3OH, CH3CHO, CH3OCHO, CH3OCH3, and CH3CN are observed (Cazaux et al. 2003).
Paper: Chemical Evolution of Some Selected Complex Organic Molecules in Low-mass Star-forming Regions
Authors: Bratati Bhat, Rumela Kar, Suman Kumar Mondal, Rana Ghosh, Prasanta Gorai, Takashi Shimonishi, Kei E. I. Tanaka, Kenji Furuya, Ankan Das
Figure caption: Abundance variation of CH3OH, CH3CHO, CH3O-CHO, C2H5OH, HCCCHO, CH3OCH3, and CH3CN shown with source luminosity. The red circle represents the value obtained from the RD, and the blue circle represents the same obtained from MCMC. The solid black squares represent the same calculated using upper limits. The plus sign (magenta) represents the abundance for IRAS4A 16293-2422 (22 L ⊙) taken from Cazaux et al. (2003). The vertical lines represent the error bars.
Paper: Chemical Evolution of Some Selected Complex Organic Molecules in Low-mass Star-forming Regions
Authors: Bratati Bhat, Rumela Kar, Suman Kumar Mondal, Rana Ghosh, Prasanta Gorai, Takashi Shimonishi, Kei E. I. Tanaka, Kenji Furuya, Ankan Das
Figure caption: The abundance ratios of CH3CHO, CH3OCHO, C2H5OH, HCCCHO, CH3OCH3, and CH3CN w.r.t. methanol (CH3OH) plotted with source luminosity. The red circles represent the value obtained from the RD, and the blue circles represent the same obtained from the upper limits. The plus sign (magenta) represents the abundance obtained for IRAS4A 16293-2422 (22 L ⊙) taken from Cazaux et al. (2003). Vertical lines represent the error bars.
Paper: Chemical Evolution of Some Selected Complex Organic Molecules in Low-mass Star-forming Regions
Authors: Bratati Bhat, Rumela Kar, Suman Kumar Mondal, Rana Ghosh, Prasanta Gorai, Takashi Shimonishi, Kei E. I. Tanaka, Kenji Furuya, Ankan Das
Figure caption: Excitation temperature derived from rotation diagram for methanol (in black) and acetaldehyde (in red), respectively. Vertical lines represent the corresponding errors. Kinetic temperature calculated from Table 4 using CH3CN transitions for high-temperature (solid blue) and low-temperature (dashed blue) components present in IRAS4A and SVS13A.
Paper: Chemical Evolution of Some Selected Complex Organic Molecules in Low-mass Star-forming Regions
Authors: Bratati Bhat, Rumela Kar, Suman Kumar Mondal, Rana Ghosh, Prasanta Gorai, Takashi Shimonishi, Kei E. I. Tanaka, Kenji Furuya, Ankan Das
Figure caption: FWHM (red line) and integrated intensity (black-dashed) for 96.755501 GHz transition of methanol. The vertical lines represent the error bars.
Paper: Chemical Evolution of Some Selected Complex Organic Molecules in Low-mass Star-forming Regions
Authors: Bratati Bhat, Rumela Kar, Suman Kumar Mondal, Rana Ghosh, Prasanta Gorai, Takashi Shimonishi, Kei E. I. Tanaka, Kenji Furuya, Ankan Das
Figure caption: Abundance variation of CH3OH, CH3CHO, CH3OCH3, and CH3OCHO obtained from interferometric observation. Black vertical lines represent the error bar.
Paper: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
Authors: Maria D. Kazachenko
Figure caption: Scatter plots illustrating different physical variables for confined (blue) and eruptive (red) events (>C5.0 GOES flare class). See the Appendix for details.