adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-421 b: A Hot Sub-Neptune with a Haze-free, Low Mean Molecular Weight Atmosphere
Authors: Brian Davenport, Eliza M.-R. Kempton, Matthew C. Nixon, Jegug Ih, Drake Deming, Guangwei Fu, E. M. May, Jacob L. Bean, Peter Gao, Leslie Rogers, Matej Malik
Figure caption: Comparison of the combined exoTEDRF + Eureka! transmission spectrum to Aurora retrievals (top) and various PLATON forward models (bottom). The best-fit retrieval model is shown in the top panel, with the darkness of the shading indicating the 1σ and 2σ limits, and is replotted in the bottom panel for comparison against the other forward models. The middle panel shows the absorption cross sections for key molecules, which demonstrates how the spectrum is a poor fit for both CH4 and CO2. The plotted forward models include different metallicity and C/O scenarios, as well as a water-rich composition, and the inclusion of disequilibrium SO2. Forward models incorporating equilibrium chemistry are shown with dashed lines. The “10× solar + SO2” model has 108 times the equilibrium SO2 abundance as its counterpart. Offsets have been applied to the forward models at 2.8 μm to account for the best-fit offset between the NIRISS/SOSS and NIRSpec/G395M data.
Paper: TOI-421 b: A Hot Sub-Neptune with a Haze-free, Low Mean Molecular Weight Atmosphere
Authors: Brian Davenport, Eliza M.-R. Kempton, Matthew C. Nixon, Jegug Ih, Drake Deming, Guangwei Fu, E. M. May, Jacob L. Bean, Peter Gao, Leslie Rogers, Matej Malik
Figure caption: White-light curves for NIRISS and NIRSpec observations along with model fits for each reduction method. On the right of each plot is a histogram showing residuals. The increased scatter in the Deming reduction relative to Eureka! for G395M is most likely due to different reduction choices, namely that the Deming reduction starts with rateints files and as a result does not run GLBS.
Paper: TOI-421 b: A Hot Sub-Neptune with a Haze-free, Low Mean Molecular Weight Atmosphere
Authors: Brian Davenport, Eliza M.-R. Kempton, Matthew C. Nixon, Jegug Ih, Drake Deming, Guangwei Fu, E. M. May, Jacob L. Bean, Peter Gao, Leslie Rogers, Matej Malik
Figure caption: Comparison of transmission spectra between data reductions for the NIRISS/SOSS and NIRSpec/G395M observations, including the σ-difference between our modeled transit depths.
Paper: A Two-hump Spectrum in the Prompt Emission of GRB 240825A
Authors: Hai-Ming Zhang, Zi-Qi Wang, Cui-Yuan Dai, Yi-Yun Huang, Wen-Qiang Liang, Ruo-Yu Liu, En-Wei Liang, Xiang-Yu Wang
Figure caption: The time-integrated spectrum measured from T0 + 0.529 s to T0 + 5.831 s and the model fits for GRB 240825A. Left panel: the spectral fitting with the Band+CPL model. Middle panel: the spectral fitting with the Band+BPL model. Right panel: the spectral fitting with the Band+SBPL model. The dashed lines represent the Band component, the dotted lines represent the extra component (CPL, BPL, or SBPL), and the solid lines represent the sum of them. The lower panels show the residual of the spectral fitting.
Paper: A Two-hump Spectrum in the Prompt Emission of GRB 240825A
Authors: Hai-Ming Zhang, Zi-Qi Wang, Cui-Yuan Dai, Yi-Yun Huang, Wen-Qiang Liang, Ruo-Yu Liu, En-Wei Liang, Xiang-Yu Wang
Figure caption: GBM and LAT count-rate light curves of GRB 240825A with 0.1 s time binning in different energy bands. The bottom panel shows the energies of the events above 100 MeV that have high association probability (>95%) with this GRB. The dashed red vertical lines indicate the time intervals that are selected for spectral analyses, and the blue shadow region indicates the time interval a1 when no high-energy photons are detected by Fermi-LAT.
Paper: A Two-hump Spectrum in the Prompt Emission of GRB 240825A
Authors: Hai-Ming Zhang, Zi-Qi Wang, Cui-Yuan Dai, Yi-Yun Huang, Wen-Qiang Liang, Ruo-Yu Liu, En-Wei Liang, Xiang-Yu Wang
Figure caption: The time-resolved spectrum of GRB 240825A measured from T0 + 1.901 s to T0 + 3.915 s (interval b). Left panel: the spectral fitting with the Band+CPL model. Middle panel: the spectral fitting with the Band+BPL model. Right panel: the spectral fitting with the Band+SBPL model. The dashed lines represent the Band component, the dotted lines represent the extra component (CPL, BPL, or SBPL), and the solid lines represent the sum of them. The lower panels show the residual of the spectral fitting.
Paper: A Two-hump Spectrum in the Prompt Emission of GRB 240825A
Authors: Hai-Ming Zhang, Zi-Qi Wang, Cui-Yuan Dai, Yi-Yun Huang, Wen-Qiang Liang, Ruo-Yu Liu, En-Wei Liang, Xiang-Yu Wang
Figure caption: The νFν model spectra plotted for each of the time bins considered in the time-resolved spectroscopy. The dashed lines represent the Band component, the dotted lines represent the extra component (CPL or SBPL), and the solid lines represent the best-fit model. The dashed lines represent the part above 1 GeV of the best-fit model (for intervals a2 and c), corresponding to the extrapolation of Band component.
Paper: A Two-hump Spectrum in the Prompt Emission of GRB 240825A
Authors: Hai-Ming Zhang, Zi-Qi Wang, Cui-Yuan Dai, Yi-Yun Huang, Wen-Qiang Liang, Ruo-Yu Liu, En-Wei Liang, Xiang-Yu Wang
Figure caption: Time variation of the LAT flux (top panel) and photon index (bottom panel) for GRB 240825A. The blue line shows the fit with a broken power law to the data after T0 + 3.9 s.
Paper: ALMASOP: Detection of Turbulence-induced Mass Assembly Shocks in Starless Cores
Authors: Shih-Ying Hsu, Sheng-Yuan Liu, Xunchuan Liu, Pak Shing Li, Tie Liu, Dipen Sahu, Ken'ichi Tatematsu, Shanghuo Li, Naomi Hirano, Chin-Fei Lee, Sheng-Jun Lin
Figure caption: 3 mm continuum (black contours), integrated intensity of CH3OH Eu = 7 K transition (green rasters and dotted contours), and integrated intensity of N2H+F1 = 0–1 transition (brown contours). The contour levels for N2H+ (brown) are set as follows: [5σ, 45σ, 85σ, 125σ, 165σ] for G208N2, [5σ, 17.5σ, 30σ, 42.5σ, 55σ] for G209N, [5σ, 10σ, 15σ, 20σ, 25σ] for G212N1, and [5σ, 15σ, 25σ, 35σ, 45σ] for the remaining targets. The contour levels for the 3 mm continuum (black) are set at [5σ, 15σ, 25σ, 35σ]. The contour levels for the CH3OH (green dotted) are set at [5σ, 15σ, 25σ, 35σ, 45σ]. The small ellipse in the bottom left corner represents the synthesized beam. The pink crosses marking the nearby protostellar cores within the field, from east to west, are G205.46-14.56N2 in panel (a) and HOPS 89 and HOPS 91 in panel (b).
Paper: ALMASOP: Detection of Turbulence-induced Mass Assembly Shocks in Starless Cores
Authors: Shih-Ying Hsu, Sheng-Yuan Liu, Xunchuan Liu, Pak Shing Li, Tie Liu, Dipen Sahu, Ken'ichi Tatematsu, Shanghuo Li, Naomi Hirano, Chin-Fei Lee, Sheng-Jun Lin
Figure caption: Flux density channel map of G205M3. The green raster represents CH3OH emission, the brown contours show N2H+ emission, and the black contours indicate the 3 mm continuum. The contour levels for N2H+ (brown), CH3OH (green), and 3 mm continuum (black) are set as [5σ, 35σ, 65σ, 95σ, 125σ], [5σ, 15σ, 25σ, 35σ, 45σ], and [5σ, 15σ, 25σ, 35σ]. The three segments (blue, orange, and red) illustrate the interfaces between CH3OH and N2H+ gas components having different velocity ranges. The origins of the coordinates are set at the 3 mm continuum peak position. The channel width of the observation is 0.2 km s−1. In the figure, we only presented the map for every two channels due to the limitation of the panel number.
Paper: ALMASOP: Detection of Turbulence-induced Mass Assembly Shocks in Starless Cores
Authors: Shih-Ying Hsu, Sheng-Yuan Liu, Xunchuan Liu, Pak Shing Li, Tie Liu, Dipen Sahu, Ken'ichi Tatematsu, Shanghuo Li, Naomi Hirano, Chin-Fei Lee, Sheng-Jun Lin
Figure caption: Starless core evolution simulation result. The gray rasters illustrate the regions having gas number density greater than the critical density of N2H+ (6 × 104 cm−3). The rainbow rasters illustrate the shocked (velocity jump greater than 0.2 km s−1, the sound speed) regions. The definition of the velocity jump is in Section 2. In our simulation, gas-phase CH3OH is residing in the regions having a velocity jump greater than 0.4 km s−1. The size of the box is approximately 0.16 pc.
Paper: ALMASOP: Detection of Turbulence-induced Mass Assembly Shocks in Starless Cores
Authors: Shih-Ying Hsu, Sheng-Yuan Liu, Xunchuan Liu, Pak Shing Li, Tie Liu, Dipen Sahu, Ken'ichi Tatematsu, Shanghuo Li, Naomi Hirano, Chin-Fei Lee, Sheng-Jun Lin
Figure caption: Flux density channel map of the simulated core. The purple raster and magenta contours represent CH3OH emission, the brown contours show N2H+ emission, and the black contours indicate the 3 mm continuum. The contour levels for N2H+ (brown), CH3OH (purple), and 3 mm continuum (black) are set as [30%, 50%, 70%, 90%], [50%, 70%, 90%], and [50%, 70%, 90%] of the peak flux density. The two segments (blue and red) illustrate the interfaces between CH3OH and N2H+ gas components having inconsistent velocity ranges.
Paper: ALMASOP: Detection of Turbulence-induced Mass Assembly Shocks in Starless Cores
Authors: Shih-Ying Hsu, Sheng-Yuan Liu, Xunchuan Liu, Pak Shing Li, Tie Liu, Dipen Sahu, Ken'ichi Tatematsu, Shanghuo Li, Naomi Hirano, Chin-Fei Lee, Sheng-Jun Lin
Figure caption: Channel maps of the observations and simulations. The top five rows display channel maps of the five observed fields, with source names labeled at the right of each row. The bottom three rows show channel maps of a simulated core from three different projected lines of sight. The CH3OH emission is represented in green and blue raster colors, N2H+ emission is shown as brown contours, and the 3 mm continuum is indicated by black contours. Contour levels for N2H+ and the continuum are set at [10%, 30%, 50%, 70%, 90%] and [60%, 75%, 90%] of their respective peak flux densities for each row.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Raw and binned front surfaces for disks with viable emission surfaces in 12CO J = 3–2 (blue), 13CO J = 3–2 (orange), and CS J = 7–6 (purple). The binned diffuse backside points of AA Tau, SY Cha, and LkCa 15 are shown as “x” points. Lines of constant 〈z/r〉 from 0.1 to 0.6 are shown as gray background lines. The beam size is shown in the upper right corner of each plot; the gray shaded region corresponds to everything interior to one beam size.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Peak intensity maps of 12CO J = 3–2 for all exoALMA sources made with the fiducial images. Parametric tapered power-law surfaces from DISCMINER are overlaid in white, with each contour being separated by the beam size (0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15); the bold lines represent the major and minor axes. The synthesized beam is shown in the lower left corner of each plot. The 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩30 beam cubes are plotted in the background in gray.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Peak intensities of 12CO J = 3–2 (blue), 13CO J = 3–2 (orange), and CSJ = 7–6 (pink) in kelvins for all exoALMA sources. The solid black lines show the peak intensities found with GoFish, and the points are the temperature points found using disksurf, binned by a quarter of the beam size. The error bars on the points represent the standard deviation of the temperature within each bin. The radial profiles are reported out to the molecular emission Redge radius.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Rolling emission surfaces (CS J = 7–6, pink; 12CO J = 3–2, blue; 13CO J = 3–2, orange) with continuum substructures identified by P. Curone et al. (2025). The dashed lines show the continuum gaps, and the solid lines show the continuum rings. The yellow shaded regions highlight the surface structures that overlap with continuum and or gas substructures.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Emission surface points with associated brightness temperatures; raw surface data points are shown as smaller background points. The raw data is binned by a quarter of a beam size for molecules above 20 K (larger circles) and below 20 K (triangles). The contour background shows the 2D temperature profiles calculated with Equation (5). Lines of constant temperatures at 50, 40, 30, and 20 K are shown in black.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Normalized integrated intensity for LkCa 15. The dashed vertical lines show Redge, R95, R90, and R68. Only intensity inward of Redge is used in the calculation of the total flux and respective 95th, 90th, and 68th percentile radii.
Paper: exoALMA. I. Science Goals, Project Design, and Data Products
Authors: Richard Teague, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Christophe Pinte, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Cristiano Longarini, Ryan A. Loomis, Frédéric Masset, Francois Menard, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Gallery of 13CO J = 3–2 emission from the exoALMA sources. The field of view of each panel is the same as that in Figure 1. The ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩ beam is shown in the lower left corner. The linear color scaling is set to span up to 95% of the peak value in each panel.
Paper: exoALMA. I. Science Goals, Project Design, and Data Products
Authors: Richard Teague, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Christophe Pinte, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Cristiano Longarini, Ryan A. Loomis, Frédéric Masset, Francois Menard, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Peak intensity of the CS J = 7–6 emission for all exoALMA sources. The field of view of each panel is the same as that in Figure 1. The ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩ beam is shown in the lower left corner. The linear color scaling is set to span up to 95% of the peak value in each panel.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Peak intensities derived from GoFish (black lines), disksurf (white circles), and DISCMINER (red lines). The beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩ is shown in the upper right of each plot.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Emission surface comparison between disksurf (dashed line and background points) and DISCMINER (solid blue line) for two model cubes at 30° and 60°, respectively. The model cubes are identical besides their inclination. The red line denotes the known τ = 2/3 surface. The top two panels show the results for 12CO J = 3–2, and the bottom two panels show the results for 13CO J = 3–2.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: The same as Figure 15, but for 13CO J = 3–2.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: The same as Figure 15, but for CS J = 7–6.
Paper: exoALMA. V. Gaseous Emission Surfaces and Temperature Structures
Authors: Maria Galloway-Sprietsma, Jaehan Bae, Andrés F. Izquierdo, Jochen Stadler, Cristiano Longarini, Richard Teague, Sean M. Andrews, Andrew J. Winter, Myriam Benisty, Stefano Facchini, Giovanni Rosotti, Brianna Zawadzki, Christophe Pinte, Daniele Fasano, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Mario Flock, Misato Fukagawa, Charles H. Gardner, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Francois Menard, Ryuta Orihara, Daniel J. Price, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida
Figure caption: Velocity residuals calculated with DISCMINER for J1615 (top panels) and LkCa 15 (bottom panels), derived with the disksurf parametric emission surface and the DISCMINER parametric emission surface. We subtract the velocity residuals (labeled “Residual”), and subtract the absolute value of the velocity residuals (labeled “Absolute Residual”).