adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. I. Science Goals, Project Design, and Data Products
Authors: Richard Teague, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Christophe Pinte, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Cristiano Longarini, Ryan A. Loomis, Frédéric Masset, Francois Menard, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Channel maps of 12CO emission from SY Cha (top) and HD 135344B (bottom), showing the effect of different channel widths. The channel widths, labeled at the top of each panel, correspond to 13.3, 26.4, 52.9, 105.8, and 211.5 m s−1 at the rest frequency of 12CO. Each channel was CLEANed down to 3× the rms measured in a line-free region of the image. Note that while the background noise is reduced with coarser channel widths, structures in the emission morphology can be washed out. Also note that the finest channel sampling of 15.3 kHz, the native channel spacing, is actually below the spectral resolution of the data so would suffer from considerable covariance with adjacent channels (R. A. Loomis et al. 2018).
Paper: exoALMA. I. Science Goals, Project Design, and Data Products
Authors: Richard Teague, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Christophe Pinte, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Cristiano Longarini, Ryan A. Loomis, Frédéric Masset, Francois Menard, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: 12CO emission, converted to brightness temperature using the Rayleigh–Jeans approximation, from the disk around LkCa 15, demonstrating the differences between the three different imaging sets released with the exoALMA program: “high” resolution, left; “fiducial,” center; and “low,” right. The spatial resolution and channel spacing for each image are, from left to right, 86 mas × 67 mas and 200 m s−1, ﹩0\mathop{.}\limits^{^{\prime\prime} }15\times 0\mathop{.}\limits^{^{\prime\prime} }15﹩ and 100 m s−1, and ﹩0\mathop{.}\limits^{^{\prime\prime} }3\times 0\mathop{.}\limits^{^{\prime\prime} }3﹩ and 100 m s−1. Note that the “high” resolution image sets have variable angular resolutions set by the requirement of resolving the continuum substructure.
Paper: exoALMA. I. Science Goals, Project Design, and Data Products
Authors: Richard Teague, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Christophe Pinte, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Cristiano Longarini, Ryan A. Loomis, Frédéric Masset, Francois Menard, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Combined analyses of the gas structure and dynamics with the dust substructure can provide insights into the physical processes sculpting the disk. These four panels display emission from the disk around RXJ1604.3-2130 A with (a) showing the dust continuum reported by P. Curone et al. (2025), (b) the 12CO peak intensity, and (c) the inferred projected velocity, v0, with A. F. Izquierdo et al. (2025) describing the techniques used to calculate these. Panel (d) shows the residual velocity structure after subtracting a purely Keplerian model, revealing substantial deviations that can be associated with pressure variations (J. Stadler et al. 2025; C. T. Yoshida et al. 2025).
Paper: exoALMA. I. Science Goals, Project Design, and Data Products
Authors: Richard Teague, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Christophe Pinte, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Cristiano Longarini, Ryan A. Loomis, Frédéric Masset, Francois Menard, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Example of the peak intensities derived from the “fiducial set” of images for HD 135344B. All panels share a 4″ × 4″ field of view centered on the star. The spatial resolution of molecular emission images is ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩ and the channel spacing is 100 m s−1 for both 12CO and 13CO and 200 m s−1 for CS. The continuum image has a synthesized beam of 90 mas × 76 mas with a position angle of 85﹩\mathop{.}\limits^{^\circ }﹩.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Nonparametric (data points) and parametric surfaces (solid and dashed curves) for 12CO J = 3–2. The larger black points represent radially binned data. We exclude two disks (HD 135344B and J1604) whose surfaces could not be extracted due to a face-on geometry. Background gray lines show scale heights (z/r) from 0.1 to 0.6 with 0.1 increments. The darker blue solid line shows the tapered power-law surface fit from DISCMINER, and the light blue and gray dashed line shows the tapered power-law fit from disksurf, which uses the background data points. The gray cross markers for AA Tau and SY Cha show the diffuse outer surface points that we do not include in the parametric fits.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Rolling surfaces made from the raw r − z disksurf emission surface points for 12CO J = 3–2 (blue), 13CO J = 3–2 (orange), and CS J = 7–6 (pink). Vertical dashed lines denote emission surface substructure, whose identification is discussed in Section 5. We label dips in the emission surfaces with the nomenclature first used in C. J. Law et al. (2021a), where “Z” denotes a dip in the emission surface, followed by the radial location in astronomical units . We also plot the continuum rings (solid gray lines) and gaps (dashed gray lines) identified in P. Curone et al. (2025). Thin background gray lines show scale heights (z/r) from 0.1 to 0.6 with 0.1 increments. The beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩ is shown in the upper right corner for each disk. AA Tau is zoomed in to better show structure.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Top panel: Average z/r in 12CO for disks with moderate inclination, plotted against M* (leftmost plot), average 12CO brightness temperature (middle plot), and the outer radius of the gaseous disk (rightmost plot). The points are colored by brightness temperature at 100 au. Background gray points are literature values from previous studies. Bottom panel: Average z/r in 12CO for disks with moderate inclination, plotted against disk mass calculated via the rotation curve from C. Longarini et al. (2025; leftmost plot), disk mass calculated via the dust mass from P. Curone et al. (2025; middle plot), and disk mass calculated using N2H+ from L. Trapman et al. (2025; rightmost plot). Points that represent exoALMA sources are colored by the 12CO Redge. Smaller gray points are MAPS sources with mass measurements from P. Martire et al. (2024), S. M. Andrews et al. (2018), and L. Trapman et al. (2025). The Pearson correlation coefficient, rp, or the Spearman correlation coefficient, rs, is shown in the top right of each figure. When a linear function is fit, the results are plotted, and the equation is shown in the top left of each figure. Disk labels: AA Tau = 1, CQ Tau = 2, DM Tau = 3, HD 143006 = 5, HD 34282 = 6, J1615 = 8, J1842 = 9, J1852 = 10, LkCa 15 = 11, MWC 758 = 12, PDS 66 = 13, SY Cha = 14, V4046 Sgr = 15. Disks without retrievable surfaces are excluded.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: The same as Figure 9, but for 13CO J = 3–2. The orange solid line shows the tapered power-law surface fit from DISCMINER, and the gray and peach dashed line shows the tapered power-law fit from disksurf.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: The same as Figure 9, but for CS J = 7–6. The purple solid line shows the tapered power-law surface fit from DISCMINER, and the gray and lavender dashed line shows the tapered power-law fit from disksurf.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Peak intensities derived from GoFish for disks with identified intensity structure. Intensity bright spots are marked with solid lines and labeled with a “B,” and intensity dips are marked with dashed lines and labeled with a “D.” Several bright spots and gaps are unlabeled due to overlap; we refer the reader to Table 4 for the full list of radial locations. Blue corresponds to 12CO, orange corresponds to 13CO, and pink corresponds to CS. Proposed planet locations, discussed in C. Pinte et al. (2025), are shown at their suggested radial locations in green. Continuum rings and gaps, identified and discussed in P. Curone et al. (2025), are shown as gray solid lines (rings) and dashed lines (gaps).
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Nonparametric surface points used to calculate the 2D temperature in r − z space. The color of the points corresponds to the difference between the observed brightness temperature (Tobs) and the temperature found by the 2D fit (Tfit). The boxed numbers in the upper right corners represent the absolute value of the average ﹩\frac{{T}_{{\rm{obs}}}-{T}_{{\rm{fit}}}}{{T}_{{\rm{obs}}}}﹩; values closer to zero indicate the 2D fit more closely matches the observed temperature structures.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Integrated intensity profiles for 12CO J = 3–2. The shaded regions represent the upper and lower uncertainties. The beam size of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 is shown in the top right corner.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Two channel maps of V4046 Sgr at 2.00 and 3.70 km s−1. The left column shows two channels with no points overlaid, and the right column shows the channels with the raw emission surface points identified by disksurf. There is a notable gap in the emission surface points that is not visible in the channels.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Line centroid map residuals of the disk velocity relative to its rotation from raw 12CO (3–2) predictions of disks unstable to the VSI, MRI, and GI, assuming a perfect background subtraction of the disk rotation. The raw images have a 26 m s−1 velocity resolution. From left to right, different disk inclinations are shown. The models consider only the upper (or front) disk hemisphere, and the disk rotation is counterclockwise in the sky. The color bar limits have been adjusted for each instability.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Line centroid map residuals of the disk velocity relative to its rotation from 12CO (3–2) predictions of turbulent protoplanetary disks, including the effects of the spatial resolution (35 mas FWHM Gaussian beam), the spectral resolution (104 m s−1 channel spacing), and the sensitivity of exoALMA. We show the resulting velocity deviations from a modified Keplerian model for a geometrically thick disk, fitted to the line centroid map using EDDY. The disk models consider only the upper (or front) 12CO layer, and the disk rotation is counterclockwise in the sky. From top to bottom, we show unstable disks with active VSI, MRI, and GI. From left to right, different disk inclinations are shown. The beam size is displayed in the lower left corner of each panel. A 5σ clipping was applied to all moment maps. The color bar limits have been adjusted for each instability.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Cartesian view of the disk perturbations at Z ∼ 2.5H for the HD (top), MHD (middle), and SGHD (bottom) simulations, with active VSI, MRI, and GI, respectively. Shown are, from left to right, perturbations in the gas density, radial velocity, meridional velocity, and azimuthal velocity. The color bar limits are adjusted for each instability.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Selected channel maps from 12CO (3–2) predictions of disks unstable to the VSI, MRI, and GI, for a disk inclination of 30°. The left 2.5 panels show the raw product, while the right 2.5 panels include the effect of the spatial resolution (35 mas FWHM Gaussian beam), spectral resolution (104 m s−1 channel spacing), and sensitivity of exoALMA. The models only consider the upper (or front) CO layer.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Polar view of the disk perturbations at Z ∼ 2.5H for the HD (top), MHD (middle), and SGHD (bottom) simulations, with active VSI, MRI, and GI, respectively. From left to right, we show perturbations in density, radial velocity, meridional velocity, and azimuthal velocity. The color bar limits are adjusted for each instability.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: 12CO (3–2) line centroid map residuals and selected channel maps from synthetic predictions of an MRI-unstable disk for a disk with an inclination of 60°, highlighting a localized feature. The images include the effect of the spatial resolution (35 mas FWHM Gaussian beam, shown in the lower left corner), spectral resolution (104 m s−1 channel spacing), and sensitivity equivalent to that of exoALMA.