adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Left to right: fiducial 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 CLEAN, 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 RML, 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩05 RML, and native RML (no restoring beam) images. We show each image product for the continuum-subtracted 12CO J = 3–2 emission in J1842 at v = 5.2 km s−1, with each panel plotted on an independent color scale. While beam convolution is not necessary in the RML imaging process, it can be useful to enable more direct comparisons between CLEAN and RML, as well as for constraining the resolution of the RML images. Beam-convolved images are also necessary for compatibility with some analysis software (e.g., tasks that require information about the restoring beam, which does not exist in the native RML image).
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 2, but for SY Cha. Shown are three adjacent channels, centered at v = 3.6 km s−1 where the 12CO J = 3–2 non-Keplerian feature appears most prominently.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Zoomed-in view of the 12CO J = 3–2 NKFs present in the RML (left) and CLEAN (right) images for each source. The color bars are in units of Jy arcsec−2.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 2, but for HD 135344B. As HD 135344B displays large NKFs that persist throughout the cube, we show three adjacent and representative channels centered at v = 6.6 km s−1.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 2, but for J1604. As J1604 displays large NKFs that persist throughout the cube, we show three adjacent and representative channels centered at v = 4.5 km s−1.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 2, but for J1842. Shown are three adjacent channels, centered at v = 5.2 km s−1 where the 12CO J = 3–2 non-Keplerian feature appears most prominently.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 2, but for LkCa 15. Shown are three adjacent channels, centered at v = 6.9 km s−1 where the 12CO J = 3–2 non-Keplerian feature appears most prominently.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 2, but for J1615. Shown are three adjacent channels, centered at v = 3.9 km s−1 where the 12CO J = 3–2 non-Keplerian feature appears most prominently.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: 12CO J = 3–2 observations from the Atacama Large Millimeter/submillimeter Array (ALMA), continuum emission, and near-infrared scattered light images for the five newly detected planet candidates. The first row shows the 12CO J = 3–2 channels with the identified velocity kinks. The second row presents the corresponding peak intensity map. The third row displays a high-pass filtered peak intensity map using a Gaussian kernel twice the size of the beam, where we overlay the location of the planetary wake, derived using the same thermal structure as in the phantom models and projected vertically onto the CO-emitting surface. The fourth row shows the exoALMA continuum (P. Curone et al. 2025), and the last row presents SPHERE dual-beam polarimetric imaging observations. The white circles indicate the velocity kinks shown in Figure 2, while the blue dot marks the deprojected location on the disk midplane. No SPHERE data are available for AA Tau, as it is currently too faint to lock the adaptive optics system.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Sources displaying large-scale non-Keplerian arcs. For each object, we show the channel at systemic velocity (central column), as well as channels at two velocity offsets on the blue side of the line (first two columns) and the opposite channels on the red side of the line (last two columns). Solid lines indicate the expected location of the isovelocity curves at Keplerian velocities ±100 m s–1. White arrows indicate deviations from the expected isovelocity curves for Keplerian rotation, and white circles highlight velocity kinks, i.e., distortions of the isovelocity curves. The beam is indicated as a gray circle and the horizontal white line is a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 scale. The color map traces the square root of the intensity between zero and the peak. Note that the ringlike structure seen in CQ Tau is the continuum emission.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Sources with velocity kinks consistent with embedded planets (white circles). White arrows indicate additional deviations from Keplerian rotation. Beams and scales as in Figure 1.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Evidence for complex CO abundance distributions. The white arrows in the first and last columns show regions where the upper and lower surfaces merge, indicating desorption. In the central two columns, the orange arrows show that the emission between the upper and lower surfaces is always greater than the emission between the near and far sides of the upper isovelocity curves (red arrows with dotted line), even if the projected separation is similar. The beam is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩25. The color map represents the log of the intensity to highlight low-brightness regions.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Emission surfaces for 12CO J = 3–2 and 13CO J = 3–2 for J1615 and SY Cha found using the CLEAN cubes and the RML cubes. Raw r − z points are shown in purple for the CLEAN data and in aqua blue and red for the RML data. The larger points show the binned surfaces. The horizontal dashed lines show the maximum surface radius, ﹩{r}_{\max }﹩. The beam size of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 is shown in the upper left corner.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Sources showing a filamentary pattern between the emission surfaces (indicated by white arrows). Note that such patterns are also visible in SY Cha, J1615, and LkCa 15, as shown in Figure 2. A potential kink in the isovelocity is shown with a white circle. Beams and scales as in Figure 1.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Radial temperature profiles, found using the disksurf surface points, for 12CO J = 3–2 and 13CO J = 3–2 for J1615 and SY Cha using the CLEAN and RML cubes. The larger points show the temperatures binned by a quarter of the beam size. The beam size of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 is shown in the upper left corner.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Sources with smooth, Keplerian-looking, velocity structure, or with signal-to-noise ratio too low to extract reliable structures at the considered scales. Beams and scales as in Figure 1.
Paper: exoALMA. VIII. Probabilistic Moment Maps and Data Products Using Nonparametric Linear Models
Authors: Thomas Hilder, Andrew R. Casey, Daniel J. Price, Christophe Pinte, Andrés F. Izquierdo, Caitlyn Hardiman, 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, Iain Hammond, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan Loomis, Ryuta Orihara, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Top: peak velocity maps v0 extracted from the benchmark model synthetic data, using both the conventional method (left; see Section 2.5) and our method (right). The right-most panel shows the true benchmark model line-of-sight velocities v0, truth. The v0 maps also show isovelocity contours spaced by 200 m s−1, and the beam is shown in the top left panel. The second row shows the difference between the recovered v0 maps and the truth. Our method debiases the v0 map and recovers the full amplitude of the substructures. Bottom: same as above except showing recovered peak intensity maps I0.
Paper: exoALMA. VIII. Probabilistic Moment Maps and Data Products Using Nonparametric Linear Models
Authors: Thomas Hilder, Andrew R. Casey, Daniel J. Price, Christophe Pinte, Andrés F. Izquierdo, Caitlyn Hardiman, 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, Iain Hammond, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan Loomis, Ryuta Orihara, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Best-fitting nonparametric (NP) model cube fit to the benchmark model synthetic data, which has a 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 beam and noise comparable to the data. The top row shows synthetic data. The second row shows the best fit after beam convolution (beam plotted in top left). The third row shows the best fit without beam convolution. The fourth row shows the ground truth for comparison. We see that the model can resolve intensity gradients smeared by the beam. The fifth row shows the residual between the synthetic data and the convolved model. The sixth row shows the residuals between the model and ground truth. The residuals show that the model reconstructs the true intensity distribution up to the noise, except for in the central two beams or so.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison of 12CO observations of LkCa 15 and J1615 (left column) with synthetic channel maps with various amounts of freeze-out depletion, from full freeze-out (i.e., CO abundance is 0 where the temperature is below 10 K) to no freeze-out (i.e., CO abundance is the same as in the disk surface: 10−4, even where T < 20 K). For both sources, we used the best hydrodynamical model from Figure 7. The color map scales with the log of the brightness temperature to highlight the emission from the disk midplane where the models differ. The green checkmarks indicate the models that visually best reproduce the observations.
Paper: exoALMA. X. Channel Maps Reveal Complex 12CO Abundance Distributions and a Variety of Kinematic Structures with Evidence for Embedded Planets
Authors: Christophe Pinte, John D. Ilee, Jane Huang, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Richard Teague, 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, Caitlyn Hardiman, Thomas Hilder, 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, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison of 12CO J = 3–2 ALMA observations (top row) with synthetic channel maps from our 3D hydrodynamics calculations with embedded planets of 1, 2, 3, and 5 MJup (from top to bottom). The channel width is 0.1 km s−1. Synthetic maps were convolved to a Gaussian beam to match the spatial resolution of the observations. Orange dots show the location of the sink particles: central star and planet. The Δv value indicates the offset from systemic velocity. The green checkmark indicates the models that visually best reproduce the observations.