adsabs/AstroCLIMB huggingface dataset:
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:  13CO 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 points with connecting lines in between them. The vertical dashed and solid blue 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.
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 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.
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 for all sources including the ones for CS J = 7–6. For most sources, the CS rotation curves rotate faster than their CO counterparts, further providing evidence for vertical stratification since the CS molecular line emitting height is located closer to the colder midplane and thus shows faster rotation than the CO molecules located at the upper warm irradiated surface layers. The innermost two beam sizes from the center 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. The reference Keplerian rotation is plotted as a thin dashed–dotted line for each molecule. The beam sizes for each molecular line are plotted in their respective color 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:  12CO δυϕ profiles for selected sources focused on the region of the continuum emission with highlighted radial locations of pressure substructures (red vertical lines). From Figure 1, we expect dust rings and gaps to be colocated with negative (⊖) and positive (⊕) δυϕ gradients if caused by pressure maxima and minima, respectively. The vertical gray shaded areas show the width of the continuum rings (P. Curone et al. 2025). The other plot annotations are the same as in Figure 5.
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 deviations from Keplerian rotation extracted from a 3D hydrodynamical simulation (R. Teague et al. 2019). The dashed black true mean δυϕ line is taken directly from the hydrodynamical simulation. The colored δυϕ lines are extracted from the hydrodynamical data, projected onto the sky, with the discminer approach then applied (see Equation (6). The different lines correspond to a planet at different azimuthal locations (ϕpl) in the disk measured counterclockwise from the redshifted disk major axis.
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 ﹩\partial \mathrm{ln}{P}_{\mathrm{mid}}/\partial \mathrm{ln}{\rm{R}}﹩ for selected sources, focused on the region of their continuum substructures. The vertical colored arrows in the upper left show variations in the stellar mass of ±3%, which would result in a shift of the whole profiles up and down. We expect dust rings and gaps to be colocated with ﹩\partial \mathrm{ln}{P}_{\mathrm{mid}}/\partial \mathrm{ln}R﹩ = 0 if induced by pressure maxima and minima (see Figure 1(b)). The vertical gray shaded areas show the width of the continuum rings (P. Curone et al. 2025). The other plot annotations are the same as in Figure 5.
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Integrated line and continuum fluxes, scaled to a distance of 150 pc, of the disk sample examined in this work (in green, blue, and purple) combined with 20 class II disks from the AGE-PRO ALMA large program, shown in black (D. Deng et al. 2025; C. Agurto-Gangas et al. 2025). C18O (2–1) and (3–2) observations are denoted as circles and stars, respectively. The C18O (3–2) fluxes are reduced by a factor of 2.3, the median C18O (3–2)/C18O (2–1) line ratio of models with Mdisk ≥ 10−4 M⊙ from L. Trapman et al. (2025). Herbig disks are highlighted with a pink circle. Triangles show upper limits, with open triangles representing upper limits in both N2H+ and C18O.
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 the logarithmic midplane pressure derivative for all sources with temperature profiles focused on the region of the continuum emission using the high-resolution images. The vertical colored arrows in the upper left show variations in the stellar mass of ±3%, which would result in a shift of the whole profiles up and down. We expect dust rings and gaps to be colocated with ﹩\partial \mathrm{ln}{P}_{\mathrm{mid}}/\partial \mathrm{ln}R﹩ = 0 if induced by pressure maxima and minima (see Figure 1(b)). The vertical gray shaded areas show the width of the continuum rings (P. Curone et al. 2025). The beam sizes for each molecule are plotted in the lower-right corner in their respective color.
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: Same as Figure E7 but focused on the disk region beyond the continuum emission using the high-surface-brightness sensitivity images. The dashed–dotted vertical line shows the radius enclosing 95% of the continuum emission (P. Curone et al. 2025) and the dotted vertical line indicates the scale radius Rc for a D. Lynden-Bell & J. E. Pringle (1974) Σ profile derived by C. Longarini et al. (2025).
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 and  13CO radial profiles of δυϕ using the high-surface-brightness sensitivity images. Same as Figures 4 and E3, but here showing δυϕ in units of kilometers per second.
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Gallery of the new ALMA Band 6 and 7 observations presented in this work. Colors are peak-normalized for each individual panel. For each source the 285 GHz continuum is shown first, with its N2H+ (3–2) integrated intensity map shown directly below that. Note that the last two panels show the Band 6 225 GHz and C18O (2–1) observations of RXJ 1842.9-3532. White (except for C18O) and pink contours denote 5σ and 3σ, respectively. The white contours for C18O also show 3σ.
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Gas disk mass posteriors obtained from fitting either 13CO, C18O, N2H+, and the 225 GHz continuum for the T Tauri disks (shown in blue) or 13CO, C18O, and the 225 GHz continuum for the Herbig disks (shown in purple). In green we show the posteriors of gas disk masses derived from the disk kinematics by B. Veronesi et al. (2021), P. Martire et al. (2024), and C. Longarini et al. (2025). Gas mass upper limits from kinematics, taken to be 5% of the stellar mass (e.g., S. M. Andrews et al. 2024; B. Veronesi et al. 2024), are shown as a green vertical dashed line.
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 the CO line-width residuals for the whole sample focused on the region of the continuum emission using the high-resolution images.
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 the CO peak intensities for the whole sample focused on the region of the continuum emission using the high-resolution images.
Paper: Biases from Missing a Small Planet in High Multiplicity Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Matthias Y. He
Figure caption: Top: histograms of the difference in gap complexity (left), mass partitioning (center), and impact parameter dispersion (right) of individual systems in L24 once a planet has been removed. The gap complexity sample is a stacked histogram of cases when an edge planet is removed (blue) and when a middle planet is removed (orange). Bottom: the same as the top for the change in system metrics between SysSim’s synthetic underlying and detected samples. The gap complexity sample is now split between cases when all planets removed are edge planets (blue) vs. cases when at least one middle planet is removed (orange). The systems in the bottom right panel have been downselected to include only the transiting planets in the SysSim catalogs.
Paper: Biases from Missing a Small Planet in High Multiplicity Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Matthias Y. He
Figure caption: Cumulative distribution functions of gap complexity (top), mass partitioning (bottom left), and impact parameter dispersion (bottom right) for a sample of 80 4+ planet L24 systems. The solid lines (dark blue) represent the observed systems, while the dotted lines (light blue) represent the sample of systems with a planet removed. In the top right panel, the One Planet Removed sample is split between systems with an edge planet removed (light blue) and systems with a middle planet removed (purple).
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Emission line-based gas disk masses vs. dust masses for the 19 sources examined in this work plus the 20 class II disks from the AGE-PRO ALMA large program (C. Agurto-Gangas et al. 2025; D. Deng et al. 2025; L. Trapman et al. 2025; K. Zhang et al. 2025). Note that the 1.3 mm flux used to derive the dust mass is very likely at least somewhat optically thick for the brightest sources, so dust masses ≳20 M⊕ should be considered lower limits of the true dust mass. Gray dashed lines show gas-to-dust mass ratios of 10, 100, and 1000.
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Comparison of the gas mass posteriors for the six Herbig disks for cases where N2H+ is excluded from the fit and xCO kept fixed (in orange) and where N2H+ is included in the fit and xCO is a free parameter (in blue). Diamonds and lines above the distribution shows its median value and 16th and 84th quantiles.
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Comparison of the gas mass posteriors obtained using models with (in red) and without (in blue) inner dust cavities. Diamonds and lines above the distribution shows its median value and 16th and 84th quantiles.
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Posterior distributions of the cosmic-ray ionization rate (ζmid), obtained by refitting the observation using the kinematically measured gas mass and its uncertainties as a prior. Diamonds and lines above the distribution shows its median value and 16th and 84th quantiles.