adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: Image of a portion of M51; RGB = F1800W/F1130W/F560W (18 μm, 11.3 μm, 5.6 μm). Areas where we have obtained complete 1–28 μm spectroscopy are indicated. Expanded cutouts are Brα (4.05 μm) images of these areas. Spectra have been extracted for the four r = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩75 circular regions shown in the cutouts.
Paper: The Exoplanet Edge: Planets Do Not Induce Observable Transit Timing Variations with a Dominant Transit Timing Variation Period Faster than Half Their Orbital Period
Authors: Daniel A. Yahalomi, David Kipping, Eric Agol, David Nesvorný
Figure caption: Hypothetical perturbing planet periods in single-planet systems from T. Holczer et al. (2016) with TTVs (ΔBIC > 6) if the observed TTVs are (left) upper and (right) lower exoplanet edge TTVs. Marker size is indicative of TTV amplitude.
Paper: Contribution of Alfvénic Waves on the Formation and Deflection of Switchbacks: Insights from Two Decades of WIND Spacecraft Data
Authors: Hui Li, Fanzhuo Dai, Chi Wang, Wence Jiang, Haoyu Li
Figure caption: Comparison of Alfvénicity and plasma parameters of the switchback with the surrounding solar wind. (a)–(c) The ratio of Alfvén wave fraction fAW, Alfvén wave purity ﹩\overline{{E}_{rr}}﹩, and the average instability growth rate of parameters γ/ω0 for switchback compared to the surrounding solar wind before and after the switchback. The horizontal axis represents five time intervals: Pre-2 (two intervals before the event), Pre-1 (one interval before the event), Event (the switchback interval itself), Post-1 (one interval after the event), and Post-2 (two intervals after the event). The black dashed line represents the average level of the entire solar wind. (d)–(h) The distribution of ratios of the average value measured during the switchback to that measured in the surrounding solar wind, for proton density, proton temperature, magnetic field strength, total pressure, and plasma β, respectively. (i) The distribution of the relative shear speed of the solar wind during the switchbacks. The two values on the left side of each subplot represent the mean and the median, respectively.
Paper: Contribution of Alfvénic Waves on the Formation and Deflection of Switchbacks: Insights from Two Decades of WIND Spacecraft Data
Authors: Hui Li, Fanzhuo Dai, Chi Wang, Wence Jiang, Haoyu Li
Figure caption: Overview of switchbacks identified before and after a high-speed stream. (a) Switchback occurrence rate per unit distance, OR. (b) Magnetic field intensity, ∣B∣ (blue), and solar wind speed, ∣VSW∣ (red). (c) Time-frequency distribution of Err.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Shifted spectra for each annulus. In each panel, the spectra are plotted as a function of velocity from the line center and azimuthal angle in the disk coordinate. The numbers in the upper-left corner indicate the radius of the annulus in arcseconds.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: (Left) Radially averaged azimuthally stacked spectra at ﹩r=0\mathop{.}\limits^{{\rm{^{\prime\prime} }}}4-0\mathop{.}\limits^{{\rm{^{\prime\prime} }}}8﹩. The stacked azimuthal range is limited to one-quarter of an annulus, and the center azimuthal angle is shown in the legend. The gray solid lines indicate the fiducial model spectrum. (Right) Residual of observed spectra after subtracting the fiducial model. Note that the spectra are vertically shifted for visibility purposes. The blue-shaded area indicates the optically thick line cores.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Corner plot of the CO line fitting at ﹩r=0\mathop{.}\limits^{{\rm{^{\prime\prime} }}}6﹩.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Observed continuum images, best-fit model images, and relative error between the observations and model images. The white ellipses on the left column indicate the observational beam size. The error maps are masked by the 3σ noise level measured in the observation images.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Teardrop plots for different inclinations. The wing feature persists despite 5° differences in the input inclination. Unlike Figure 2, the velocity convolution is not applied for completeness.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: (Left) Integrated intensity map of the C18O J = 2–1 line. The white dotted circle indicates the dust ring location. The white solid circle shows the beam size. (Right) Radial profile of the peak brightness temperature. The black bar indicates the beam size.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Two-dimensional temperature structure constructed by using the best-fit parameters of the spectral model fitting.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Local specific intensity field along the disk vertical axis in a unit of brightness temperature.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: The same as Figure 2 but the Gaussian function is adopted for the opacity profile.
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Overview of the four sources studied in this work, shown on the same spatial scale for the dust (top two rows) and gas (bottom row). Top: millimeter dust continuum as observed within the exoALMA program (P. Curone et al. 2025). Middle: micron-sized dust observed through NIR scattered light with SPHERE (T. Stolker et al. 2017; J. de Boer et al. 2021; B. B. Ren et al. 2023). The SPHERE images are normalized to the peak value and shown with a logarithmic normalization of the color map to emphasize the structures in the outer disk. To highlight the location of the crescents, two continuum contours around the peak of the dust asymmetries are overlaid on the dust images. Bottom: peak intensity of the 12CO J = 3–2 emission line with overlaid continuum emission (five contour levels equally placed between 3σ and the peak flux). Note the larger spatial scale of the gas vs. dust images.
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Velocity residuals Δv0 after subtraction of the Keplerian model from the data, shown for 12CO and 13CO J = 3–2 and all four targets. For HD 34282, only emission from the top side of the disk was considered when making the v0 map, following the procedure described in A. F. Izquierdo et al. (2025). The beam is shown in the bottom left corner of the top row. The red-blue circle and arrow in the bottom right corner of the second row indicate the underlying rotation pattern of each disk. To highlight the location of the crescents, two continuum contours around the dust asymmetries are overlaid on the images.
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Analytical model of a vortex, described as elliptic streamlines of constant velocity with a Gaussian velocity profile. The first two panels show the absolute velocity of the vortex in both the vortex frame and sky frame. The last panel depicts the velocity projected along the line of sight, showing a complex morphology purely resulting from the projection. In the last two panels, the underlying disk geometry is overlaid as gray contours, corresponding to a position angle of 243 ° and inclination of 16 ° (same as for HD 135344B).
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Line-of-sight velocity of the analytical vortex model, shown for different disk geometries and vortex parameters. The parameters given on top of the figure correspond to the morphology shown in the first panel. In the top of each individual panel, the parameters changed compared to this base vortex model are given. The underlying disk geometry is overlaid as gray contours.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Left panel: surface density Σ in LkCa 15 of the stratified models in comparison with the isothermal model when solving for the scale-height using both the 12CO and 13CO emitting height at the same time. Right panel: comparison between the temperatures returned by the solution shown in the left panel and the temperature fit reported in M. Galloway-Sprietsma et al. (2025; at three different layers, the extrapolation to the midplane and the values at the emitting heights of 12CO and 13CO). Bottom panel: comparison between the emitting heights of 12CO and 13CO, showing that in the inner disk the former is smaller than the latter.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Like Figure 3, but we now show the results of the stratified model in comparison with the results of the isothermal model. We consider two cases, described in detail in the main text, in which we set the temperature based either on the brightness temperature of the line or on the fitted disk temperature profile in the midplane. For the isothermal model, solid lines are for 12CO while dashed lines are for 13CO.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Top panel: density profiles in LkCa 15 at 80 au. We show the density profiles for the stratified case and for the two isothermal cases described in Section 5.1. The stratified profile is normalized to 1 in the midplane, and the other two profiles are normalized so that at the 12CO emitting height (marked by the dashed vertical line) they intersect with the stratified one. Bottom panel: temperature profile derived from the M. Galloway-Sprietsma et al. (2025) fit.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison between the mass inferred using the 12CO emitting height and the mass inferred using the 13CO emitting height. The gray solid line marks where the two masses are the same. The red lines are the results of the power-law fit described in the main text.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: CO depletion factors needed with respect to the ISM value xCO = 10−4 to match the masses derived in this work from 13CO with the kinematical masses derived in C. Longarini et al. (2025) and P. Martire et al. (2024).
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Masses derived from the isothermal model, assuming either the temperature in the midplane or the temperature at the emitting height, in comparison with the stratified case for the whole sample.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison between the masses measured with various methods, namely, the dynamical masses derived from the rotation curve (P. Martire et al. 2024; C. Longarini et al. 2025), the emitting heights (this work), and (moderately) optically thin C18O (K. Zhang et al. 2021) for the disks in our sample.