adsabs/AstroCLIMB huggingface dataset:
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Left panel: periods of excited ℓ = 1 g modes as a function of the effective temperature, with the palette of colors (right scale) indicating the logarithm of the e-folding time (τ e in years), for the PG 1159 sequence with M ⋆ = 0.530M ⊙. In this case, the effective temperature and its uncertainties (horizontal segments) correspond to the spectroscopic determination of Werner et al. (2011). Right panel: same as left panel, but for ℓ = 2 modes. In both panels, the pulsation periods with the identification of ℓ according to our asteroseismic model (see Table 7) are shown as horizontal segments, where their widths represent the possible T eff interval, according to spectroscopy (Table 8).
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Left panel: periods of excited ℓ = 1 g modes as a function of the effective temperature, with the palette of colors (right scale) indicating the logarithm of the e-folding time (τ e in years), for the PG 1159 sequence with M ⋆ = 0.542M ⊙. Right panel: same as left panel, but for ℓ = 2 modes. In both panels, the pulsation periods with the identification of ℓ according to our asteroseismic model (see Table 7) are shown as horizontal segments, where their widths represent the possible T eff interval, according to spectroscopy (Table 8).
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: Spectra from the three Chandra observations of Her X-1 high state, focusing on the Fe K band. The data are fitted with a simple spectral model consisting of a power law plus two Gaussians, shown in blue. The red dashed lines show the positions of Fe I (6.4 keV) and Fe XXV (6.67 keV) transitions. The super-orbital phase ϕ of each Chandra observation is given below its ID.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Internal chemical profile of the asteroseismic model of PG 1159−035 (M ⋆ = 0.565M ☉, T eff = 129, 600 K) in terms of the outer fractional mass. The locations of the O/C and O/C/He chemical interfaces are indicated with gray regions.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Radial density profiles of the ambient environments in the models of Group B. The red solid, yellow long-dashed, green dashed, blue dashed–dotted, and magenta dotted lines are associated with models B1, B2, B3, B4, and B5, of which the mass-loss rates of the progenitor are ﹩\dot{M}={10}^{-4},\,5.0\,\times {10}^{-5},\,{10}^{-5},\,5.0\times {10}^{-6},\,{10}^{-6}\ {M}_{\odot }\,{\mathrm{yr}}^{-1}﹩, respectively. The total mass loss is 8 M ⊙ for each model, and the gas density in the outer region is fixed at n ISM = 0.1 cm−3.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: (a) Shock radius, (b) velocity, and (c) shocked gas mass as a function of age for Group A compared with the observation data of Type Ia SNRs shown by the data points. The red solid, yellow dashed, and green dotted lines show the model results for models A1, A2, and A3, of which the ISM densities are n ISM = 10, 0.1, and 10−3 M ⊙ yr−1, respectively.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Time evolution of the broadband nonthermal spectra from models in Group A for each emission component until the radiative phase. Snapshots at t = 50 yr, 500 yr, 5000 yr, and ﹩3{t}_{\mathrm{tr}}﹩ (or 3 × 105 yr for model A3) are shown from left to right, and models A1, A2, and A3 (n ISM = 10, 0.1, and 10−3 cm−3, respectively) from top to bottom. The emission components include synchrotron (blue solid), nonthermal bremsstrahlung (green dashed–dotted), inverse Compton (magenta dashed), and π 0-decay (red dotted).
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Same as Figure 5, but for models in Group B overlaid with CC SNR observation data. The line formats are the same as in Figure 6.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Same as Figure 4, but for the models in Group B. ﹩\dot{M}={10}^{-4},{10}^{-5},{10}^{-6}\ {M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ are shown from the top to the bottom, which are for models B1, B3, and B5, respectively. The ages plotted are 200, 450, 600, and 50,000 yr in B1; 200, 2300, 4000, and 50,000 yr in B3; and 200, 2600, 7000, and 50,000 yr in B5. Gray lines in the rightmost panels show the total component in model A2 at the age of 50,000 yr.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Time evolution of the luminosities in three energy bands for models in Group A compared to the observation data of Type Ia SNRs (data points). The line formats are the same as in Figure 3. Shown are the luminosities (a) at 1 GHz, (b) from 1 to 100 GeV, and (c) from 1 to 10 TeV.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Radial profiles of the magnetic field strength in the ambient environments of the models in Group B. The line formats are the same as in Figure 1.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Same as Figure 3, but for Group B, overlaid with the results from models in Group A in gray lines and CC SNR observation data for reference. The line formats are the same as in Figure 1.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: The HCN J = 2 → 1 and HCO+ J = 2 → 1 spectra of 17 galaxies observed with the APEX 12 m telescope. Solid and dashed lines show the line profiles of HCN J = 2 → 1 and HCO+ J = 2 → 1, respectively. We detect both lines in 12 galaxies. Five sources only have one detected line with a velocity-integrated line intensity >3σ. The nondetections are tagged as “ND” above the line labels.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: OTFMAP polarimetry data reduction flowchart. The raw data are combined in sets of four HWP PAs within a sky rotation tolerance of 3°. The sets are reduced using CRUSH, which generates a scan per ﹩{ \mathcal R }﹩ and ﹩{ \mathcal T }﹩ arrays and per HWP PA. Then, these scans are zero-level background corrected and combined, from which Stokes parameters are derived. After the Stokes parameters are corrected for IP, the scans are sky rotated and flux-calibrated. Finally, all Stokes parameters from different legs, flights, and/or cycles are merged to compute the final images, which contain Stokes IQU; polarization fraction, P; position angle, PA, of polarization; and polarized intensity, PI. The pipeline computes uncertainties and covariances, which are taken into account during all stages of the data reduction.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Flux variation and aircraft altitude as a function of time for the observations of M83 at 154 μm. (a) Measured peak fluxes of the scans per HWP PA and ﹩{ \mathcal R }﹩ and ﹩{ \mathcal T }﹩ arrays. (b) PWV-corrected fluxes using the fits shown in Figure 5. The mean (black solid line) and 2σ uncertainty (black dotted line) are shown. (c) Aircraft altitude at the time of data acquisition. The PWV during the observations of M83 (green for F731 and cyan for F735 shadowed regions) is shown in Figure 4.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: Using different distributions (left: normal, right: power law) of optical depth (τ) values, we generated model observation sets to compare with our real VLBA observations. Intrinsic radio luminosities (red circles) were calculated from the jet-dominated radio-to-X-ray relation (blue dotted line from Figure 5). The real observation sets are presented as blue squares where the points within boxes are nondetections. The calculated model observation set are presented here in orange (normal) and yellow (power law) triangles. The mean values of optical depth and the percentages of matching in total set, detection, and nondetection only are shown as well. With a similar mean value of ∼10, a random power-law distribution of absorption (optical depth) parameter yields a better agreement with the observed detections (≈71%) and nondetections (≈65%) than a normal distribution.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: Left: comparison between 6 cm radio peak luminosities and 2–10 keV X-ray luminosities similar to that shown in Figure 5. Right: FP described by Dong et al. (2014) as shown in the right panel of Figure 6, but different lines of optical depth or opacity (tau, τ) are drawn assuming that all AGNs have the same intrinsic radio/X-ray ratio and that synchrotron self-absorption leads to the large dispersion seen.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: PWV variation as a function of time for the flights associated with M83 at 154 μm (see Figure 3). Top panel: expected PWV for flight F735. The PWV during the observations of M83 (cyan shadowed region) is shown. Bottom panel: expected PWV for flight F731. The PWV during the observations of M83 (green shadowed regions) is shown.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Example of flux variation as a function of time and aircraft altitude for M82 at all HAWC+ bands. Peak fluxes (first and third row) of the scans per HWP PA and ﹩{ \mathcal R }﹩ and ﹩{ \mathcal T }﹩ arrays at 53 μm (top left), 89 μm (top right), 154 μm (bottom left), and 214 μm (bottom right) of M82. The aircraft altitude (second and fourth rows) at the time of data acquisition is shown. The vertical lines show the boundaries between different flights.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: Plot of radio-loudness vs. Eddington ratio for our VLBA sample and the local Seyferts studied by Panessa & Giroletti (2013). The symbols are the same as those in the previous two figures.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: The FP described by Merloni et al. (2003; left) and by Dong et al. (2014; right) using peak radio luminosities. The symbols are the same as those in Figure 5. The red dashed line on the right panel represents the classical division between RL and RQ AGNs by Terashima & Wilson (2003).
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Results of the Spearman rank correlation analysis for the 17 optical emission-line parameters and global properties and the 18 SimBAL absorption-line and derived properties. The symbols have the same meaning as in Figure 2. The top plot shows the results for the 30 object low-redshift sample, while the middle and bottom plots show the results for the E1 < 0 and E1 > 0 subsamples, respectively. Among the optical parameters, E1 and the related parameters R FeII, [O III] equivalent width, SPCA1, E1, L Bol, and L Bol/L Edd, are most strongly correlated with the SimBAL parameters. Among the SimBAL parameters, the offset velocities and parameters associated with the volume filling fraction are the most strongly correlated with the optical parameters.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Cumulative distributions of 17 of the SimBAL parameters segregated by their E1 parameter values. Distributions that are significantly different (p < 0.05; Table 1) are shown in dark red and dark blue, while distributions that are not significantly different are shown in a pale hue of the same color. All of the outflow velocity parameters (V off, V max, V min) are shown in the top-right panel. Of the SimBAL-related parameters, those three, the thickness of the absorber, the log filling factor, the number of clouds covering the continuum-emission-line region, and the covering-fraction correction (discussed in Section 4.4) show statistically different distributions between the E1 > 0 and E1 < 0 subsets.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Results of the Spearman rank correlation analysis for the 18 SimBAL parameters. The stars show the results for a Monte Carlo scheme to estimate the effects of the errors; see Leighly et al. (2022) for details. The top plot shows the results for the whole sample, while the middle and bottom plots show the results divided by the E1 parameter. Of particular interest is the weak but significant anticorrelation between the velocity parameters and location of the outflow for E1 < 0 and the correlation for the same parameters for E1 > 0.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Location of the outflow determined using SimBAL modeling (Choi et al. 2022) and normalized by the dust sublimation radius as a function of the outflow velocity. Negative velocities denote outflows. The circles and squares show the column-density-weighted velocity, while the left and right triangles show the maximum and minimum speeds, respectively. There is an anticorrelation (correlation) between ﹩\mathrm{log}R/{R}_{{\rm{d}}}﹩ and the outflow velocity for the E1 < 0 (E1 > 0) FeLoBALQs. These different behaviors imply a difference in the formation and acceleration of outflows for the two classes of FeLoBALQs.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Ratio of the Keplerian velocity at the location of the outflow to the absolute value of the outflow velocities. The stars denote V off. The triangles show V min and V max and can be offset from the stars if the trough includes both inflow and outflow. Very large values of this ratio show absorption features that have velocities much lower than the Keplerian velocity.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: The v 0 residuals for CO, top, and CS, bottom, after subtracting a purely Keplerian background model, v kep, left column, or a pressure-supported Keplerian model, v prs, right column. In each panel, the synthesized beam is shown in the lower left, while a 100 au scale bar is shown in the lower right. The dotted contours show radial steps of 0.″5 and azimuthal steps of 30°. The colorbar shows the residuals in units of σ, with absolute residuals less than 1σ left white. The dashed contour in (d) highlights the Doppler flip.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: The deprojected velocity residuals for CO (top row) and CS (bottom row), assuming all velocities are azimuthal (left column), radial (central column), or vertical (right column). For the azimuthal and radial velocities, wedges along the minor and major axes have been masked, as here the observations are insensitive to those components. In each panel, the synthesized beam and a 50 au scale bar are shown in the bottom left and right corners. Note that the field of view for the bottom row is smaller than the top row.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Polar projections of the velocity residual maps from Figure 5 with CO after subtracting a purely Keplerian background profile in panel (a), after subtracting a pressure-supported background in panel (b), and CS after subtracting a Keplerian background profile in panel (c). In all panels, the residuals are normalized by the local uncertainty on the line center, δ v 0. The two horizontal lines in each show the gap edges of the continuum gap at 82 au (1.″35) reported by Ilee et al. (2022), coincident with the gap in scattered light (Debes et al. 2013; Rapson et al. 2015; van Boekel et al. 2017) and molecular line emission (Teague et al. 2017). The dotted boxes highlight the “Doppler flip” feature. The spirals traced by the CO are annotated. The circle marks the center of the “Doppler flip.” The dotted square marks the location of the continuum excess reported in Tsukagoshi et al. (2019). The disk rotates from right to left.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Residuals in the local line width, ΔV, when an azimuthally averaged model, ΔV avg, is subtracted for CO (panel (a)) and CS (panel (b)), normalized by the uncertainty of the linewidth measurement, δΔV. The radial profile used as the background model, ΔV avg, is shown in panel (c). In both (a) and (b), the center of the proposed “Doppler flip” is shown by the white point, while the ellipse in the bottom left shows the synthesized beam. Dotted contours show steps of 0.″5 in radius and 30° in azimuth. In (c), the shaded regions show the 1σ standard deviation in each azimuthal bin. The vertical dotted line shows the location of the gap center as reported by Ilee et al. (2022).
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Line-of-sight velocity maps, v 0, for CO (left) and CS (right). The synthesized beam is shown in the bottom left of each panel. The v 0 maps are masked where the peak intensities fall below a 5σ level for CO and a 3σ level for CS.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Radial velocity perturbations driven by planets of different masses: 1 M Nep, 1 M Sat, and 0.5 M Jup, shown in panels (a), (b), and (c), respectively. Each panel is centered on the putative planet’s location, with the dotted line showing the orbital radius of the planet, 82 au. The solid contours mark 100 m s−1, the velocity traced by CS emission. The cross marks the center of the disk. Each panel spans a field of view of 2.″5 (150 au). The analytical models were calculated following Bollati et al. (2021).