adsabs/AstroCLIMB huggingface dataset:
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Top: cloud mass evolution for a destroyed cloud simulation. The solid blue line shows the total amount of cloud gas in the volume relative to the initial cloud mass (78 M ⊙). The dashed blue line is an estimate of the total cloud mass that has been carried out of the volume (described in Section 3.2). Bottom: dust mass evolution for a = 0.1 μm grains in a destroyed cloud simulation. The solid red line is the total amount of dust in the simulation volume relative to the initial dust mass (0.78 M ⊙). The red dashed line is an estimate of the dust mass that has been carried out of the simulation. The solid black line is the total amount of dust sputtered. The black dashed and dotted–dashed lines show the total amount of dust sputtered in T < 106 K and T ≥ 106 K, respectively. Overall, after 2.9 Myr (0.29 t sp,w), the cloud has been almost completely mixed into the wind and 24% of the initial dust mass is sputtered, while the rest has been carried out of the simulation volume.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Cloud (top) and dust (bottom) mass evolution for a survived cloud simulation with a = 0.1 μm dust grains. See Figure 4 for a full description of this figure. The initial cloud and dust masses are 6.2 × 103 M ⊙ and 63 M ⊙, respectively. As the cloud evolves, it accretes rapidly cooled gas from the mixed phase and grows in mass. Essentially no sputtering is seen in the ∼80 Myr (5.6 t sp,w) duration of the simulation.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Simulation domain for our large cloud simulations. Here, we simulate a 100 pc radius cloud in a box that is 128 r cl long at a fixed resolution of r cl/64 cells (d x = 1.5625 pc). The box sizes for our other setups can be found in Table 1.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Dust mass evolution for the same simulation setup described in Figure 4, but with a = 0.01 μm dust grains. After roughly 3 Myr, 12% of the simulation’s original dust content has exited the box, while 76% of the dust is destroyed after mixing into T ≥ 106 K gas, and 12% of the dust is destroyed in cooler gas. The wind sputtering time for a = 0.01 μm grains is 1 Myr.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Top panel: 11 ms snapshot. First two panels show individual emissivities (ϵ) of ν  e  and ﹩{\bar{\nu }}_{e}﹩. Absolute values of the emissivities are highest near the disk. The rightmost panel shows ﹩\tfrac{{\epsilon }_{{\nu }_{e}}}{{\epsilon }_{{\bar{\nu }}_{e}}}﹩. At these early times, ﹩{\epsilon }_{{\nu }_{e}}﹩ can be up to ∼4 orders of magnitude greater than ﹩{\epsilon }_{{\bar{\nu }}_{e}}﹩ close to the disk. Geometry wise, ﹩{\epsilon }_{{\nu }_{e}}﹩ has a different structure than ﹩{\epsilon }_{{\bar{\nu }}_{e}}﹩. As one moves away from the disk toward the poles, the individual emissivities drop, and ﹩{\epsilon }_{{\bar{\nu }}_{e}}﹩ dominates over ﹩{\epsilon }_{{\nu }_{e}}﹩. Bottom panel: 65 ms snapshot. The emissivities decrease with time for both ν  e  and ﹩{\bar{\nu }}_{e}﹩. The bottom right panel also shows that the emission structure has changed as compared to 11 ms case. Compared to the 11 ms case, the geometric emission structure of ν  e  and ﹩{\bar{\nu }}_{e}﹩ are more similar. ﹩{\epsilon }_{{\nu }_{e}}﹩ still dominates over ﹩{\epsilon }_{{\bar{\nu }}_{e}}﹩ close to the disk, but now the ratios differ by at most 1 order of magnitude near the disk. As explained in the text, this emission structure for 11 and 65 ms are crucial for determining the presence of crossings.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Evolution of the crossings as a function of angle from the pole. The discretized radial distance of a neutrino packet is set to be 60–70 km. In the top panel, the left plot is at the equator and the right plot is 60° below the pole (30° above the equator). Clear crossings are present at and 30° above the equator. As one moves farther above the disk as shown in the bottom panels, the crossings disappear, and ν  e  distribution overwhelms ﹩{\bar{\nu }}_{e}﹩. Crossings have already disappeared by the time the neutrinos are 45° from the equator. The titles of the plot (c), (f), (g), and (h) correspond to the respective spatial locations labeled in Figure 1 as one moves up from the equator.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Angular distribution of ν  e  and ﹩{\bar{\nu }}_{e}﹩ across the disk at t ∼ 65 ms. ﹩\cos \theta ﹩ is defined with respect to the radial direction so that ﹩\cos \theta =1﹩ are neutrinos moving radially outwards. We find robust crossings between the ν  e  and ﹩{\bar{\nu }}_{e}﹩ distributions across the entire disk between r ∼ 20 and 120 km beyond which the radiation field turns off. The titles of the plot (a), (b), (c), (d), and (e) correspond to the respective spatial locations labeled in Figure 1.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Density and electron fraction of the simulation at t ∼ 11 ms and t ∼ 65 ms. The text labels in the 65 ms Y  e  plot are the locations where the representative crossings analysis are shown in Figures 2 and 3.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Top panel: 11 ms snapshot. At these early times, ﹩{\kappa }_{{\nu }_{e}}﹩ is many orders of magnitude greater than ﹩{\kappa }_{{\bar{\nu }}_{e}}﹩ in a funnel-shaped region around the disk. Bottom panel: ∼65 ms snapshot. ﹩{\kappa }_{{\nu }_{e}}﹩ and ﹩{\kappa }_{{\bar{\nu }}_{e}}﹩ become more similar, but ﹩{\kappa }_{{\nu }_{e}}﹩ is still about 1–2 orders of magnitude greater than ﹩{\kappa }_{{\bar{\nu }}_{e}}﹩ near the disk.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Origin locations (r cyl, z) of ν  e s and ﹩{\bar{\nu }}_{e}{\rm{s}}﹩ that are present in the r = 60 km, θ polar = 45° control volume at 11 and 65 ms. For both of the time snapshots, most of the emission happens very close to the disk as can be seen from the z origin.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Crossings at 45° and polar regions for the 11 ms snapshot. Compared to the results at t ∼ 65 ms where the crossings only occur close to the disk, they occur ubiquitously for earlier times.
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Lagrangian derivative of Y  e  due to emission or absorption of neutrinos for 11 ms (top) and 65 ms (bottom). Blue regions correspond to an increase in Y  e  and red for a decrease. Averaged over the azimuthal angle ϕ and in time from 0 to 20 ms (top) and 50 to 70 ms (bottom).
Paper: The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Payel Mukhopadhyay, Jonah Miller, Gail C. McLaughlin
Figure caption: Locations in the r−θ plane where regions hosting crossings are shaded in green. As explained in the text, crossings are ubiquitous at early times (∼11 ms) but then evolve to only occur closer to the disk as time evolves (∼65 ms).
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: Left: right singular vectors of the original sensitivity matrix at the four corners, organized from largest to smallest singular value. The y-axis represents the five rigid body motions of M2, the five motions of the camera, bending modes of M1M3, and bending modes of M2. The color map reflects the respective units of each degree of freedom, measured in micrometers or arcseconds. Right: singular values associated with each mode. A distinct set of singular values is significantly lower, corresponding exclusively to the rigid body motions.
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: The 20 M1M3 bending modes used in the Rubin Observatory’s AOS, arranged sequentially from left to right and top to bottom. The arrangement starts with the lowest-order mode at the top-left corner. Notably, the first 19 modes appear in direct sequence, whereas the last mode, placed at the bottom right, is specifically the 27th mode. This mode is included over others in the sequence due to its significantly greater impact on wave-front alterations. The disk-shaped discontinuities visible in several modes are the result of the boundary between the primary and tertiary mirrors.
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: The 20 M2 bending modes used in the Rubin Observatory’s AOS, arranged sequentially from left to right and top to bottom. The arrangement starts with the lowest-order mode at the top-left corner. Notably, the first 17 modes appear in order, whereas the last three modes, placed at the bottom right, are specifically the 25th, 26th, and 27th bending modes. These modes are included over others in the sequence due to their significantly greater impact on wave-front alterations.
Paper: Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan
Figure caption: Grayscale FUV image stamps of all 18 galaxies detected in the UVIT survey are shown. The optical morphology in the SDSS r-band is superimposed on the image stamps. The three levels of the blue contours represent 10σ, 5σ, and 1.5σ threshold levels above the background noise. The surface brightness of the outermost contour is 24.14 mag arcsec−2. The identity numbers mentioned on each image correspond to Table 2. We mark the centroids of FUV and r-band observation with cyan and red crosses, respectively.
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: Left: right singular vectors of the rescaled sensitivity matrix at the four corners, organized from largest to smallest singular value. The y-axis represents the five rigid body motions of M2, the five motions of the camera, bending modes of M1M3, and bending modes of M2. The color map reflects the respective units of each degree of freedom, measured in micrometers or arcseconds. Right: singular values associated with each mode.
Paper: Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan
Figure caption: Left panel: ratio of FUV SFRs (aperture radius = 1.″5/Petrosian aperture) vs. Δ(FUV − r). Right panel: distribution of Δ(FUV − r) and D fil. The color bar shown in the image represents the stellar mass of individual filament galaxies. The horizontal lines enclose the region representing flat color gradient galaxies.
Paper: Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan
Figure caption: Histogram showing the distribution of log(sSFRFUV) for detected/detected+undetected filament galaxies (hatched blue/dashed cyan), a sample of cluster galaxies from RedMaPPer catalog (filled red; Rykoff et al. 2016), and Coma cluster (unfilled red; Hammer et al. 2010). The galaxies fall in the same stellar mass range.
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: Sensitivity matrix in the corner R00 of the Rubin Observatory focal plane. Due to the scaling difference between the effect of hexapod motions and bending modes, they have been split in two.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: The comparison of the nonparametric SFH reconstructed by our fiducial model (Section 2.4), plotted as dashed lines, with the SFH derived from a parametric delayed-tau model, plotted as solid lines (the best-fit) and shaded regions (1σ uncertainty).
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Similar to Figure 17, but now comparing with the nonparametric SFH reconstructed using the Dirichlet prior.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Comparisons of stellar-mass and SFR measures from different SFHs for the individual structural components of the six galaxies presented in this work. Color-coding is the same as Figure 6 in the main text (C1 are in red). Symbols used for individual galaxies are the same as Figure 9 in the main text. The black solid line in each panel marks the one-to-one relationship.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Comparison of the coadded SFH of individual structural components with the SFH derived from SED fitting of integrated flux. The y-axis shows the relative difference, i.e., (coadded—integrated) / integrated, of the two SFHs. The gray shaded region shows 1σ uncertainty.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Similar to Figure 13, but for the five medium-band NIRCam filters used by JEMS.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: Musca observed by Planck. Left: B-field map. The length of the line segment is proportional to the polarization fraction P with a 10% reference. Center: column density. Right: dust temperature. The half-power beamwidth of the maps ﹩5^{\prime} ﹩ is shown by the red circle in the lower left corner. The gray contours are 3.7 × 1021 cm−2. The black rectangle enclosing the southern section of the filament is the area of interest for further analysis.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: Musca. Upper: minimum alignment size by RATs calculated from our model for Musca. Lower: comparison of the polarization fraction from our model (thick solid lines) with observation data. The gray curves show P vs. r for radial cuts along the filament’s spine from observational data (see Section 3.1.2). Green dots represent the mean values of the observational P at a certain value of r. The color curves show polarization fractions from our model with different ﹩{a}_{\max }﹩. The rapid increase of alignment size toward the filament center causes the decrease of the model polarization fraction and successfully reproduces the observed polarization hole.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. (a) B-field orientation map observed at 214 μm wavelength by SOFIA/HAWC+. The black lines show the orientation of the B-field vector and are overplotted on the intensity map. The vector spacing equals the beam size, shown by a solid red circle in the lower left corner. Three regions, north, BN-KL, and south, are labeled. (b) The column density map, and (c) the dust temperature map. The light green, dark blue, and violet contours correspond to P = 0.6%, 1.0%, 1.4%. The star indicates the location of BN-KL, and the triangle shows the location of the Trapezium cluster.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. Variations of the polarization fraction, P, with the column density N(H2) (a), dust temperature T d (b), and angle dispersion function ﹩{ \mathcal S }﹩ (c). The blue, red, green, and orange dots represent the north, BN-KL, south, and the H II region, and the lines are the results of fits to power-law models, respectively.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: Musca. Variations of P, ﹩{ \mathcal S }﹩, ﹩P-{ \mathcal S }﹩, and T d as a function of the radial distance (r) constructed using RadFil by sampling radial cuts every 0.1 pc along the spine (similar to Figure A1). The radial distance is then defined as the projected distance; the negative distance is to the left, and the positive is to the right. Thin gray lines show the radial cuts, and the mean values are shown as dot makers per bin size of 0.1 pc.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. The dependence of column density on dust temperature (a), the angle dispersion function ﹩{ \mathcal S }﹩ on the column density N(H2) (b) and dust temperature T d (c), and the dependence of the ﹩P-{ \mathcal S }﹩ on the dust temperature T d (d). The blue, red, green, and orange dots represent the data in the north, BN-KL, south, and the H II regions, respectively, and the solid curves show the running mean values of the data.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. The polarization fraction maps, (a) from observation and (b)–(e) from numerical modeling: (b) ﹩{P}_{\mathrm{mod}}^{\mathrm{ideal}}﹩ without RAT-D, (c) ﹩{P}_{\mathrm{mod}}^{\mathrm{ideal}}﹩ with RAT-D, (d) ﹩{P}_{\mathrm{mod}}﹩ without RAT-D, and (e) ﹩{P}_{\mathrm{mod}}﹩ with RAT-D. The gray contour corresponds with four subregions defined in Figure 2. The star indicates the location of BN-KL, and the triangle shows the location of the Trapezium cluster.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: (Top) mean spectra, (middle) rms spectra, and (bottom) velocity-binned time lags (in the observed frame) for IC 4329A in seasons 2020–2022. In the bottom panels, the numbers in gray represent the peak ICCF coefficient ﹩{r}_{\max }﹩ in each velocity bin. In each bin, the point’s velocity is assigned as the centroid velocity weighted by the rms fluxes. The dashed horizontal lines with gray shaded bands show the time lags and uncertainties from the integrated Hβ light curves. The gray open points show velocity bins with ﹩{r}_{\max }\lt 0.5﹩, which indicates that the time lags might be unreliable. The flux densities are in units of 10−14 erg s−1 cm−2 Å−1.