adsabs/AstroCLIMB huggingface dataset:
Paper: Anisotropic Turbulent Flows Observed in Above-the-loop-top Regions during Solar Flares
Authors: Xiaoyan Xie, Chengcai Shen, Katharine K. Reeves, Bin Chen, Xiaocan Li, Fan Guo, Sijie Yu, Yuqian Wei, Chuanfei Dong
Figure caption: V-map for the whole fan area (a) and different heights (b)–(f) indicated by B0 to B4 in Figure 2, where the white disk corresponds to the speed of plasma motions <18 km s−1. The time period for v-maps is from 15:19:54 to 16:08:42 UT during the flare decay phase with the formation of the supra-arcade fan and the manifestations of upflows and downflows traveling through the fan. The histogram (probability density) of θ (θ is calculated by ﹩\arctan (\frac{{v}_{y}}{{v}_{x}}﹩) and takes the direction of upward and downward-moving flows into account within the range of 0–2π) for the v-map is included in each panel. The gray circles moving outward indicate probabilities of 0.2, 0.4, and 0.6, respectively.
Paper: Anisotropic Turbulent Flows Observed in Above-the-loop-top Regions during Solar Flares
Authors: Xiaoyan Xie, Chengcai Shen, Katharine K. Reeves, Bin Chen, Xiaocan Li, Fan Guo, Sijie Yu, Yuqian Wei, Chuanfei Dong
Figure caption: Density distribution (a), vy distribution overlaid with velocity vectors (b), v-maps for the whole area (c), and different heights (d)–(f) from the MHD simulation with the same data set as in C. Shen et al. (2022). Panels (a) and (b) are at time t = 5.5t0, and panels (c)–(g) are accumulated from t = 5.5t0 to t = 7t0 during which turbulent flows have been developed in the system. The corresponding height areas in (d)–(g) are indicated by b0 to b3 in (a). The corresponding histograms with the same direction definition as in Figure 3 for v-maps (c)–(f) are shown in (g). The gray circles moving outward indicate probabilities of 0.2, 0.4, and 0.6, respectively. As in the observations in the current Letter, we define x as the direction parallel to the loop-top, the x–y plane is the fan area, and θ is calculated by ﹩\arctan (\frac{{v}_{y}}{{v}_{x}})﹩ within the range of 0–π. The simulation uses nondimensional units with the characteristic parameters L = 1.5×1010 cm, VA = 1380 km s−1, and t0 = 108.7 s. The white dashed curve in the panel marks v = ﹩\sqrt{{v}_{x}^{2}+{v}_{y}^{2}}﹩= 18 km s−1. ﹩ \% (\frac{\pi }{4}\lt \theta \lt \frac{3\pi }{4}\,or\,\frac{5\pi }{4}\lt \theta \leqslant \frac{7\pi }{4})﹩ of All, b0, b1, and b2 is 67.1, 57.2, 65.2, and 63.0, respectively.
Paper: Anisotropic Turbulent Flows Observed in Above-the-loop-top Regions during Solar Flares
Authors: Xiaoyan Xie, Chengcai Shen, Katharine K. Reeves, Bin Chen, Xiaocan Li, Fan Guo, Sijie Yu, Yuqian Wei, Chuanfei Dong
Figure caption: AIA 131 Å observations for fan at 15:27:30 (a) and 16:03:06 (d). The arrows in panels (b) and (e) are the corresponding velocity vectors with a more yellow color indicating higher speed. Panels (c) and (f) are the v-map, where each dot indicates one pixel at 15:27:30 and 16:03:06, respectively. The white disk corresponds to the speed of plasma motions <18 km s−1. Color toward red indicates a denser distribution in the v-map. B0 to B4 in panel (d) indicates the areas for checking v-map properties at different heights of the fan in Figure 3.
Paper: Anisotropic Turbulent Flows Observed in Above-the-loop-top Regions during Solar Flares
Authors: Xiaoyan Xie, Chengcai Shen, Katharine K. Reeves, Bin Chen, Xiaocan Li, Fan Guo, Sijie Yu, Yuqian Wei, Chuanfei Dong
Figure caption: Snapshots of upflow (a) and downflow (c), whose evolution can be found in Figure 1. Arrows indicate the direction of distance increment. The dotted lines in Figures 5(a) and (c) indicate the paths used for averaging the values for the locations of the shortest and longest distances. Panels (b) and (d) display intensity and density as a function of distance of the paths shown in panels (a) and (c), respectively.
Paper: Anisotropic Turbulent Flows Observed in Above-the-loop-top Regions during Solar Flares
Authors: Xiaoyan Xie, Chengcai Shen, Katharine K. Reeves, Bin Chen, Xiaocan Li, Fan Guo, Sijie Yu, Yuqian Wei, Chuanfei Dong
Figure caption: Same as Figure 3, but we separately plot v-maps for brighter (top panels) and darker (bottom panels) turbulent flows.
Paper: Identifying Thorne–Żytkow Objects through Neutrinos
Authors: Pablo Martínez-Miravé, Irene Tamborra, Alejandro Vigna-Gómez
Figure caption: Top panels: radial evolution of the baryon density on the left and temperature on the right for different accretion rates for a steady disk. Middle panels: radial evolution of the baryon density on the left and temperature on the right for different accretion rates in the steady spherically symmetric scenario. The brown horizontal bands in the left panel highlight the regions where MSW flavor conversion is expected to take place for the solar and atmospheric neutrino mass differences and Eν ∈ [2, 100] MeV. Bottom panel: dominant mechanisms for thermal neutrino production in the plane spanned by the electron density and temperature of the medium. The shaded regions indicate the dominant processes: beta processes, electron–positron pair annihilation, plasmon decay, photoneutrino production, and bremsstrahlung (D. A. Dicus 1972; E. Braaten & D. Segel 1993; M. Haft et al. 1994; Y. Z. Qian & S. E. Woosley 1996; S. I. Dutta et al. 2004; G. Guo & Y.-Z. Qian 2016). The colored lines correspond to the density and temperature profiles for different accretion rates from 10−4 to 106 M⊙ yr−1. The star-shaped markers indicate the characteristic temperature and density of the neutron star (assumed to be constant for simplicity); the pointlike markers signal the thermodynamical quantities right outside of the neutron star (assuming a sharp boundary).
Paper: Identifying Thorne–Żytkow Objects through Neutrinos
Authors: Pablo Martínez-Miravé, Irene Tamborra, Alejandro Vigna-Gómez
Figure caption: Detection prospects of neutrinos from T﹩\dot{{\rm{Z}}}﹩Os. Left panel: sensitivity of neutrino detection from T﹩\dot{{\rm{Z}}}﹩O bursts detected by IceCube (solid lines), Super-Kamiokande (dotted lines), and Hyper-Kamiokande (dashed lines) in the plane spanned by the source distance from Earth and the signal duration. In order to guide the eye, the Milky Way edge is marked on the x-axis, together with the Large and Small Magellanic Clouds (LMC and SMC, respectively). The shaded regions correspond to a signal-to-noise ratio larger than 3 for constant accretion rates of 104 M⊙ yr−1 and 106 M⊙ yr−1 in blue and purple, respectively. Super-Kamiokande (Hyper-Kamiokande) and IceCube are sensitive to neutrino bursts from T﹩\dot{{\rm{Z}}}﹩Os lasting for ﹩\gtrsim { \mathcal O }(0.1)﹩ s within our Galaxy and beyond the Small Magellanic Cloud. Right panel: same as the left panel but for steady T﹩\dot{{\rm{Z}}}﹩Os detected by Super-Kamiokande (dotted lines), JUNO (solid lines), and Hyper-Kamiokande (dashed lines). The orange and red bands correspond to data-taking windows of 1 yr and 1 month, respectively. Super-Kamiokande and JUNO should be sensitive to the neutrino emission from steady T﹩\dot{{\rm{Z}}}﹩Os beyond the Small Magellanic Cloud for ﹩\dot{M}\gtrsim 0.1\,{M}_{\odot }﹩ yr−1.
Paper: Identifying Thorne–Żytkow Objects through Neutrinos
Authors: Pablo Martínez-Miravé, Irene Tamborra, Alejandro Vigna-Gómez
Figure caption: Top panels: expected event rate for a T﹩\dot{{\rm{Z}}}﹩O burst at 5 kpc from Earth for IceCube (left panel), Super-Kamiokande (dotted line, right panel), and Hyper-Kamiokande (dashed line, right panel). The IceCube background rate is shown as a shaded band. For Super-Kamiokande (Hyper-Kamiokande), the background rate is 10−2 s−1 (0.1 s−1) and thus not displayed. Bottom panels: expected event rate for a steady T﹩\dot{{\rm{Z}}}﹩O at 5 kpc from Earth for Super-Kamiokande (left panel) and JUNO (right panel). The background rates are displayed as shaded bands. The total and background-only event rates for Hyper-Kamiokande are analogous to the ones shown for Super-Kamiokande after accounting for the difference in fiducial volume of approximately 1 order of magnitude (and therefore not shown here).
Paper: Identifying Thorne–Żytkow Objects through Neutrinos
Authors: Pablo Martínez-Miravé, Irene Tamborra, Alejandro Vigna-Gómez
Figure caption: Diffuse flux of electron antineutrinos from T﹩\dot{{\rm{Z}}}﹩Os as a function of the neutrino energy, assuming that all T﹩\dot{{\rm{Z}}}﹩Os accrete at the same rate. The colored bands correspond to the accretion rates considered in this work, and the width of each band represents the uncertainty on the local rate of T﹩\dot{{\rm{Z}}}﹩Os (see Equation (3)). The ROI for detection coincides with the one from the DSNB searches (i.e., the white vertical band between 10 and 30 MeV). The energy threshold for IBD (the most promising detection channel) is marked by the dashed line at 1.8 MeV. For comparison, the brown band represents the DSNB computed as in P. Martínez-Miravé et al. (2024). Current searches for the DSNB already exclude the extreme scenario in which all TŻOs accrete at a rate ≳106 M⊙ yr−1.
Paper: Identifying Thorne–Żytkow Objects through Neutrinos
Authors: Pablo Martínez-Miravé, Irene Tamborra, Alejandro Vigna-Gómez
Figure caption: T﹩\dot{{\rm{Z}}}﹩O candidates (E. M. Levesque et al. 2014; E. R. Beasor et al. 2018; H. M. Tabernero et al. 2021) and potential T﹩\dot{{\rm{Z}}}﹩O progenitors in the Galaxy, as well as in the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). Potential candidates are considered to be (i) high-mass X-ray binaries in which the neutron star accretes matter from the stellar companion and unstable mass transfer is expected (H. Ge et al. 2024; T. Hutchinson-Smith et al. 2024; H. Manikantan et al. 2024) and (ii) stellar clusters where red supergiants are abundant (L. DeMarchi et al. 2021).
Paper: Identifying Thorne–Żytkow Objects through Neutrinos
Authors: Pablo Martínez-Miravé, Irene Tamborra, Alejandro Vigna-Gómez
Figure caption: Neutrino flux from a T﹩\dot{{\rm{Z}}}﹩O at 5 kpc from Earth, taking into account flavor conversion. The colored lines correspond to the accretion rates considered in this work: ﹩\dot{M}=1{0}^{-4}\,{M}_{\odot }﹩ yr−1, 10−2 M⊙ yr−1, 1 M⊙ yr−1, 102 M⊙ yr−1, 104 M⊙ yr−1, and 106 M⊙ yr−1, from bottom to top. Dashed, dotted, and solid lines correspond to electron neutrinos, electron antineutrinos, and the total flux of all neutrinos and antineutrinos, respectively. The neutrino flux increases as a function of the accretion rate, peaking at higher energies.
Paper: Anisotropic Turbulent Flows Observed in Above-the-loop-top Regions during Solar Flares
Authors: Xiaoyan Xie, Chengcai Shen, Katharine K. Reeves, Bin Chen, Xiaocan Li, Fan Guo, Sijie Yu, Yuqian Wei, Chuanfei Dong
Figure caption: V-maps for cases in A-D in X. Xie et al. (2022b). The time periods for panels (a) to (d) are 2012 October 22 12:02:09–12:40:09, 2015 June 18 01:40:08–02:20:08, 2012 July 17 15:50:08–16:20:08, and 2012 January 16 04:20:09–04:50:09, respectively. In each case, we define x as the direction parallel to loop-top and y as the direction perpendicular to the loop-top. The histogram of θ in each panel is calculated by the same approach as in the 2024 May 29 event.
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Radial profiles of δυϕ for 12CO J = 3–2 of all sources focused on the region of the continuum substructures, using the high-resolution images. The profiles are plotted starting at two beam sizes from the disk center, and the error bars show the standard deviation of each bin. The gray background gradient highlights the frank radial profiles of the dust continuum emission normalized to its peak. The locations of continuum rings, gaps, and crescents are plotted in solid, dashed, and dotted vertical gray lines, respectively (P. Curone et al. 2025). We expect dust rings and gaps to be colocated with a decreasing and increasing δυϕ profile if caused by pressure maxima and minima, respectively. The beam size is plotted in the lower-right corner. The 13CO δυϕ radial profiles can be found in Figure E4 of Appendix E.
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Radial profiles of δυϕ for 12CO J = 3–2 of all sources focused on the region beyond the continuum substructures using the high-surface-brightness sensitivity images. The error bars show the standard deviation within each extracted radial annulus. The vertical dashed–dotted line indicates the radius that encompasses 95% of the continuum emission, with the signs of the radial derivatives of δυϕ marked at this location. The beam size is shown in the lower-left corner. The 13CO δυϕ radial profiles can be found in Figure E3 of Appendix E.
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: (a) Azimuthal velocities (left axis, black lines) and midplane pressure (right axis, blue lines), (b) along with the deviations from Keplerian rotation and the first radial derivative of the pressure, for a hydrodynamic model with an imposed Gaussian gap in the pressure at R = 240 au. The pressure minimum and maximum locations are marked with vertical purple dashed and full lines, respectively. The circles in (b) mark the sign of the radial derivative of δυϕ coinciding with the pressure minimum (⊕) and maximum (⊖), respectively.
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Level of vertical stratification between the 12CO and 13CO rotation curves (see Equation (11)) outside of two beam sizes from the center. The turquoise line displays the expected isothermal velocity shift solely due to the differences in emitting height (Equation (11)).
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Rotation curves υϕ(R, z(R)) measured from 12CO (red) and 13CO (blue), shown for all sources using the high-surface-brightness sensitivity images. For radii smaller than twice the beam size, the curves are plotted with dashed lines due to uncertainties in the velocity extraction. The colored shaded area of the lines shows the standard deviation within each extracted radial annulus usually on the order of ≈10–50 m s−1. The fitted Keplerian rotation is plotted as a thin dashed–dotted line for each molecule, respectively (Equation (7)). The beam size for both molecular lines is plotted in the lower-left corner.
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Smoothed radial profiles for δυϕ (υϕ-υk) for three different sources using the three sets of continuum-subtracted image cubes at various angular and spectral resolutions These cubes are namely the high-resolution images (red, beam size < 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15), the fiducial images (turquoise, beam size = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15), and the high-surface-brightness sensitivity images (red, beam size = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩30); see R. Teague et al. (2025) for details. The colored shaded area of the lines shows the standard deviation within each extracted radial annulus. The beam sizes for each image cube are plotted in their respective color in the lower-left corner. The plot shows that the choice of imaging parameters does not negatively affect the analysis products over the scales of interest. In our cases, these are either the innermost disk regions colocated with the continuum or the global scales tracing the outermost disk radii. The δυϕ profiles agree within their uncertainties. However, caution is necessary to ensure sufficient angular resolution for rotation curve analysis; otherwise, a beam that is not sufficiently small may smear out the substructures of interest, as can be seen in the overlapping profiles.
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Radial profiles of δυϕ for  13CO J = 3–2 of all sources focused on the region of the continuum substructures, using the high-resolution images. The profiles are plotted starting at two beam sizes from the disk center, and the error bars show the standard deviation of each bin. The gray background gradient highlights the frank radial profiles of the dust continuum emission normalized to its peak. The locations of dust rings, gaps, and crescents are plotted in solid, dashed, and dotted vertical gray lines, respectively (P. Curone et al. 2025). If caused by pressure maxima and minima, then we expect dust rings and gaps to be colocated with a decreasing and increasing δυϕ profile, respectively. The beam size is plotted in the lower-right corner.
Paper: exoALMA. VI. Rotating under Pressure: Rotation Curves, Azimuthal Velocity Substructures, and Gas Pressure Variations
Authors: Jochen Stadler, Myriam Benisty, Andrew J. Winter, Andrés F. Izquierdo, Cristiano Longarini, Maria Galloway-Sprietsma, Pietro Curone, Sean M. Andrews, Jaehan Bae, Stefano Facchini, Giovanni Rosotti, Richard Teague, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption:  12CO radial profiles of δυϕ for sources with pressure substructures colocated with the continuum substructures using the high-resolution images. δυϕ substructures are labeled in each subplot as listed in Table 1. The start and end points of the substructures are annotated with black dots with connecting lines in between them. The vertical dashed and solid red lines indicate the centers of the pressure minima and maxima, respectively. The vertical gray shaded areas show the width of the continuum rings (P. Curone et al. 2025). Additional plot annotations are the same as in Figure E4.