adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Difference between the i and PA values obtained by analyzing the continuum with galario and the 12CO data with discminer (A. F. Izquierdo et al. 2025). An asinh stretch has been applied to the y-axis of the bottom panel to include the disks with a large difference in PA due to a low inclination (red circles).
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Difference between the offset in R.A. and decl. obtained by analyzing the continuum with galario and the 12CO data with discminer (A. F. Izquierdo et al. 2025).
Paper: Temporal Behavior and Latitudinal Relationships between Key Solar Parameters and Green Line Emissions in the Solar Corona
Authors: Jacob Oloketuyi, Yu Liu, Linhua Deng, Abouazza Elmhamdi, Khaled Nasser Almosabeh, Fengrong Zhu, Haitang Li, Feiyang Sha, Qiang Liu, Oladipo Emmanuel Abe, Charles Owolabi, Olufemi Olusola
Figure caption: The evolutionary trends that separately compare the sunspot numbers, F10.7 cm radio flux, and various class flares with the green line emissions captured in the solar corona (divided into high- and low latitudes). To enhance visibility, some curves have been scaled by suitable factors (as shown within the panels).
Paper: Temporal Behavior and Latitudinal Relationships between Key Solar Parameters and Green Line Emissions in the Solar Corona
Authors: Jacob Oloketuyi, Yu Liu, Linhua Deng, Abouazza Elmhamdi, Khaled Nasser Almosabeh, Fengrong Zhu, Haitang Li, Feiyang Sha, Qiang Liu, Oladipo Emmanuel Abe, Charles Owolabi, Olufemi Olusola
Figure caption: Cross-correlation analysis curves for sunspot numbers, F10.7 cm, and the various flare classes at high latitudes (first row panels) and at low latitudes (second row panels). The lag is presented in the unit of months.
Paper: Temporal Behavior and Latitudinal Relationships between Key Solar Parameters and Green Line Emissions in the Solar Corona
Authors: Jacob Oloketuyi, Yu Liu, Linhua Deng, Abouazza Elmhamdi, Khaled Nasser Almosabeh, Fengrong Zhu, Haitang Li, Feiyang Sha, Qiang Liu, Oladipo Emmanuel Abe, Charles Owolabi, Olufemi Olusola
Figure caption: The evolutionary trends of: flare events of various classes (panel (a)), the green line emissions at different latitudes (panel (b)), and sunspot numbers with F10.7 cm radio flux (panel (c)). The X-class flare curve, in panel (a), is scaled by a factor of 10 for better visualization.
Paper: Temporal Behavior and Latitudinal Relationships between Key Solar Parameters and Green Line Emissions in the Solar Corona
Authors: Jacob Oloketuyi, Yu Liu, Linhua Deng, Abouazza Elmhamdi, Khaled Nasser Almosabeh, Fengrong Zhu, Haitang Li, Feiyang Sha, Qiang Liu, Oladipo Emmanuel Abe, Charles Owolabi, Olufemi Olusola
Figure caption: The multitaper (MTM) analysis decomposes the green line emissions, F10.7 cm radio flux, sunspot numbers, and the solar flare eruptions between 1996 and 2024 to illustrate the patterns. The analysis was conducted with confidence levels of 99%.
Paper: Constraints on Nonthermal Pressure at Galaxy Cluster Outskirts from a Joint SPT and XMM-Newton Analysis
Authors: Arnab Sarkar, Michael McDonald, Lindsey Bleem, Mark Bautz, Bradford A. Benson, Priyanka Chakraborty, Catherine E. Grant, Christine Jones, Florian Kéruzoré, Eric D. Miller, Scott Randall, Charles Romero, Taweewat Somboonpanyakul, Yuanyuan Su
Figure caption: Top left: SPT y-map of the galaxy cluster AS0520. Top right: quiescent particle-background-subtracted X-ray count image of AS0520 in the 0.7–1.2 keV energy band, obtained using XMM-Newton. The solid green and dashed cyan circles represent R200 and R500, respectively, for AS0520. Bottom left: y-parameter profile extracted from the SPT-SZ map of AS0520. Bottom right: similar to the bottom left figure, but showing the X-ray surface brightness profile of AS0520 in the 0.7–1.2 keV energy band. The surface brightness profile is exposure corrected and background subtracted. In both bottom panels, the best-fit curves, as shown in solid red, are obtained by fitting only in range (0.15R500–R200). We extended the best-fit curve, as shown in dashed red. Vertical dashed and dashed–dotted lines represent the R500 and R200 of AS0520, respectively. Horizontal blue dashed lines indicate the respective instrumental background.
Paper: Constraints on Nonthermal Pressure at Galaxy Cluster Outskirts from a Joint SPT and XMM-Newton Analysis
Authors: Arnab Sarkar, Michael McDonald, Lindsey Bleem, Mark Bautz, Bradford A. Benson, Priyanka Chakraborty, Catherine E. Grant, Christine Jones, Florian Kéruzoré, Eric D. Miller, Scott Randall, Charles Romero, Taweewat Somboonpanyakul, Yuanyuan Su
Figure caption: Best-fit gas properties of galaxy clusters in our sample. Top left: the scaled best-fit electron density profiles. Green shaded region represents density profiles of 67 high-redshift SPT clusters within (0.3 < z < 1.3) (F. Ruppin et al. 2021). Top right: scaled best-fit deprojected temperature profiles. Bottom left: scaled deprojected pressure profiles. Bottom right: scaled entropy profiles. Dotted line shows self-similar entropy profile (G. M. Voit et al. 2005). In all panels, yellow shaded regions represent gas properties for the X-COP sample of clusters with redshift z < 0.1 (V. Ghirardini et al. 2019). In the top right, bottom left, and bottom right panels, gray shaded regions show the gas properties of high-redshift (z >  1.2) SPT clusters (V. Ghirardini et al. 2021).
Paper: Constraints on Nonthermal Pressure at Galaxy Cluster Outskirts from a Joint SPT and XMM-Newton Analysis
Authors: Arnab Sarkar, Michael McDonald, Lindsey Bleem, Mark Bautz, Bradford A. Benson, Priyanka Chakraborty, Catherine E. Grant, Christine Jones, Florian Kéruzoré, Eric D. Miller, Scott Randall, Charles Romero, Taweewat Somboonpanyakul, Yuanyuan Su
Figure caption: Top left: baryon depletion factor (red) and stellar fraction (green) profiles as obtained from M. Angelinelli et al. (2022). Blue curve shows the universal gas fraction. Black star represents the universal gas fraction used for the X-COP sample. Top right: nonthermal pressure fraction profiles for 1ES 0657, AS0520, AS1063, and AS0592. The blue and cyan dashed curves show the nonthermal pressure fractions predicted from the numerical simulations of K. Nelson et al. (2014) and D. Eckert et al. (2019), respectively, with their 1σ uncertainties. The black data points show the nonthermal pressure obtained for the X-COP sample of clusters. Bottom: similar to top right, but for A2744, A3404, RXCJ0232, and RXCJ2031 clusters.
Paper: Constraints on Nonthermal Pressure at Galaxy Cluster Outskirts from a Joint SPT and XMM-Newton Analysis
Authors: Arnab Sarkar, Michael McDonald, Lindsey Bleem, Mark Bautz, Bradford A. Benson, Priyanka Chakraborty, Catherine E. Grant, Christine Jones, Florian Kéruzoré, Eric D. Miller, Scott Randall, Charles Romero, Taweewat Somboonpanyakul, Yuanyuan Su
Figure caption: Top left: hydrostatic mass profiles of the clusters derived using best-fit pressure and density profiles and assuming hydrostatic equilibrium. Top right: gas mass profiles of the sample of clusters using best-fit density profiles and assuming a spherical geometry. Bottom left: the gas mass fraction profiles of the sample of clusters. Blue horizontal shaded region shows the Planck universal baryon fraction Ωb/Ωm (Planck Collaboration et al. 2016).
Paper: Little Red Dots Are Tidal Disruption Events in Runaway-collapsing Clusters
Authors: Jillian Bellovary
Figure caption: Rates of TDEs for models by N. C. Stone et al. (2017; blue) and F. P. Rizzuto et al. (2023; red). Fiducial models shown in thick lines. Top: TDE rate vs. black hole mass, with fixed velocity dispersion of σ = 40 km s−1 (thick solid lines), σ = 150 km s−1 (dashed lines), and with stellar density nstar = 106M⊙ pc−3 (dotted lines). Light gray lines extending from the fiducial blue model indicate the rate in the instance of a transition from a full to empty loss cone, for various values of the critical mass Mc. Bottom: TDE rate vs stellar velocity dispersion, with fixed black hole mass of 104 M⊙ (thick solid lines), 105 M⊙ (dashed lines), 103 M⊙ (dotted–dashed lines), and stellar density nstar = 106M⊙ pc−3 (dotted lines).
Paper: Little Red Dots Are Tidal Disruption Events in Runaway-collapsing Clusters
Authors: Jillian Bellovary
Figure caption: Comoving number density of runaway collapse black hole seeds vs redshift. Predictions from numerical simulations vary based on whether a delayed cooling model is used with supernova feedback (blue line) or not (orange line; M. Habouzit et al. 2017). Analytic predictions using variable seed masses are shown in the gray shaded area (B. Devecchi et al. 2012). Data points represent JWST LRD observations from J. E. Greene et al. (2024; green dots), D. D. Kocevski et al. (2024; red stars), and V. Kokorev et al. (2024; black diamonds). The data are ∼4 orders of magnitude below the predicted densities.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Flux-based radii (i.e., radii enclosing 68% of the emission) of 12CO, 13CO, and dust compared with the dynamical scale radii Rc. The orange squares are the exoALMA sources, while the blue ones are the MAPS. The black line shows when the flux radius is equal to the dynamical one, and the brown line is the average value for the sources.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison between the observed and the predicted radius enclosing the 90% of the 12CO emission, according to Equation (9). The gray crosses show the results assuming the CO depletion obtained by L. Trapman et al. (2024).
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Top panels: rotation curves of LkCa 15 (red dots) with the best-fit model (blue lines) and residuals according to Equation (A13). The black dashed line represents the location of the scale radius Rc. Bottom panel: non-Keplerian contribution to the rotation curve, where δvz is the correction due to the finite height of the emission, δvp is the pressure gradient, and δvd is the self-gravitating contribution.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Dynamical masses against dust masses as computed in P. Curone et al. (2025) for the exoALMA and MAPS sources. The black line shows the Mdyn = 100Mdust and the brown line the Mdyn = 400Mdust.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: αS for the exoALMA and MAPS sources, computed according to Equation (10) and comparison with literature values.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison between dynamical disk masses (this work) and literature estimates.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Top panel: surface density and Toomre Q profiles for the four most massive disks of our sample, namely, DM Tau, HD 34282, LkCa 15, and SY Cha, excluding AA Tau because of the big uncertainties (see Appendix E). Bottom panel: Surface density and Toomre Q profiles for the other five sources, namely, J1615, J1842, J1852, PDS 66, and V4046 Sgr.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Top panel: surface density and Toomre Q profiles of AA Tau, where the error bar is computed by propagating the uncertainties on star and disk masses. Bottom panel: rotation curve of AA Tau compared to a Keplerian curve (top panel) and comparison between the nonparametric emitting layer of DISKSURF and the parametric of DISCMINER (bottom panel).
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Rotation curve of the disks within our sample (red dots) of the 12CO (left panels) and 13CO (right panels) with the best-fit model using Equation (A13).
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Corner plots for AA Tau, DM Tau, HD 34282, and J1615.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Corner plots for J1842, J1852, LkCa 15, and PDS 66.
Paper: exoALMA. XII. Weighing and Sizing exoALMA Disks with Rotation Curve Modelling
Authors: Cristiano Longarini, Giuseppe Lodato, Giovanni Rosotti, Sean Andrews, Andrew Winter, Jochen Stadler, Andrés Izquierdo, Maria Galloway-Sprietsma, Stefano Facchini, Pietro Curone, Myriam Benisty, Richard Teague, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Ian Czekala, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Caitlyn Hardiman, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Ryan A. Loomis, Francois Ménard, Ryuta Orihara, Christophe Pinte, Daniel Price, Leonardo Testi, Gaylor Wafflard- Fernandez, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Corner plots for SY Cha and V4046 Sgr.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: 12CO channel maps at vlos = 1.1 km s−1, using various combinations of hydrodynamic and radiative transfer codes (code names shown in the upper left corner of each panel). The planet, embedded and thus invisible in the channel maps, is located 45° west of south. In all models, velocity kinks (indicated with a yellow dashed square in the upper left panel) are apparent in the vicinity of the planet. The inset in the lower left quadrant of each panel shows a zoomed-in view of the velocity kink. In the inset of the top left panel, we present the isovelocity contour with a red curve. The bottom right panel shows the brightness temperature along the isovelocity contour shown in the top left panel, compared to that of the FARGO3D + mcfost model. Note that the brightness temperature of all models agree well with each other.