adsabs/AstroCLIMB huggingface dataset:
Paper: Transfer of Entropy between the Magnetic Field and Solar Energetic Particles during an Interplanetary Coronal Mass Ejection
Authors: M. E. Cuesta, G. Livadiotis, D. J. McComas, L. Y. Khoo, H. A. Farooki, R. Bandyopadhyay, S. D. Bale
Figure caption: The overview of the SEP event observed by the Parker Solar Probe on 2022 February 15. In descending order, the panels include the spectrogram of energetic protons observed by HET-A, the magnetic field (RTN components in blue, green, and yellow, respectively, and its magnitude in black), the thermodynamic kappa of energetic protons observed between 10–60 MeV, and the overall intermittent kappa via two methods: ratio of moments method (solid yellow line) and fitting the distribution of magnetic increments (dashed black line), each surrounded by a shadow representing their error corresponding to one standard deviation.
Paper: MeerKAT H I Observations of Low Surface Brightness/Ultradiffuse Galaxy Candidates Projected around Two Southern Loose Groups
Authors: Chandreyee Sengupta, Tom C. Scott, Hao Chen, Hyein Yoon, Yogesh Chandola, Mengtian Li, Gyula I. G. Józsa, O. Ivy Wong, Yin-Zhe Ma, Patricio Lagos, Ruta Kale, Denis Tramonte
Figure caption: Integrated H I contours overlaid on DES g-band images of the five H I-detected UDG candidates, with the galaxy group indicated at the top of each image followed by its candidate number. The column densities of the contours are as follows (from left to right): image (1) 1.7, 2.3, 16.0 × 1019 cm−2; image (2) 1.8, 4.9, 7.7, 14.3 × 1019 cm−2; image (3) 2.2 × 1019 cm−2; image (4) 2.8, 3.7 × 1019 cm−2; image (5) 1.8 × 1019 cm−2. The ellipse at the bottom left of each image shows the size and position angle of the MeerKAT synthesized beam.
Paper: Transfer of Entropy between the Magnetic Field and Solar Energetic Particles during an Interplanetary Coronal Mass Ejection
Authors: M. E. Cuesta, G. Livadiotis, D. J. McComas, L. Y. Khoo, H. A. Farooki, R. Bandyopadhyay, S. D. Bale
Figure caption: An illustration of the transfer of entropy, or degrees of freedom, from the magnetic field to energetic particles. Also depicted are energetic particles trapped and modulated by a magnetic flux tube, which may possibly be a thermal mechanism of the transport of entropy affecting the energetic particles. The boxed equation in the center describes the transport of entropy over time (G. Livadiotis & D. J. McComas 2023b).
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: Left panel: evolution of the total magnetic energy (black solid line) but also of the poloidal (red dashed line) and toroidal components (blue dotted line). Also shown with gray lines of the same type are the corresponding evolutions when no neutrinos are taken into account (no M1). Right panel: evolution of the EM luminosity during the simulation. Note the large jump when the magnetically driven wind that is emitted at the “breakout” reaches the detector at the “eruption” time and is sustained in a steady state. Shown with gray lines is the luminosity in the absence of neutrinos (no M1), highlighting that neutrinos are useful to trigger the breakout but not necessary.
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: Two-dimensional distributions in the (x, z) plane of various quantities computed in the simulations. Starting from the left, we report the inverse plasma β (i.e., the ratio of the magnetic to thermal pressures), the poloidal (bpol) and toroidal (btor) components of the magnetic field in the comoving frame, the Lorentz factor (W), and the electron fraction (Ye). While the top row refers to a time around the breakout, i.e., at t − tmer = 39.8 ms, the bottom row shows the evolution in the steady state, i.e., at t − tmer = 77.9 ms. Light-blue contours refer to different rest-mass densities (dotted, dotted–dashed, dashed, and solid lines for 1010,  1012,  1013, and 1014 g cm−3, respectively).
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: Two-dimensional distributions in the (x, z) plane of various terms contributing to the extended Bernoulli criterion in Equation (3). Shown from left to right are the extended Bernoulli criterion 1 + (h + b2/ρ)ut − bt/κ, the geodesic criterion h ut, the magnetization b2/ρ, and the magnetocentrifugal contribution bt/κ. The top row refers to the breakout time, while the bottom row refers to the steady-state stage; neutrinos are properly accounted for in these simulations; see also Figure 2.
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: Left panel: spacetime diagram of the averaged inverse plasma β (right part) and of the averaged Parker stability criterion (left part); both parts report data associated with the “disk.” Right panel: the same as in the left panel, but for the region associated with the “funnel.” Both panels show the time of “breakout” marked with a horizontal white line and blue contours for different rest-mass densities (dashed, dotted–dashed, and solid lines for 1014,  1013.5, and 1013 g cm−3; the last can be taken to mark the surface of the HMNS).
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: Left panel: evolution of the ejection rest-mass rate ﹩{\dot{M}}_{{\rm{ej}}}﹩, showing first the peak of the dynamical ejecta and subsequently that the cooling by neutrinos reduces the efficiency of ﹩{\dot{M}}_{{\rm{ej}}}﹩ (the color shading is the same as in Figure 1). After eruption, however, the mass ejection rate increases thanks to the launching of the magnetically driven winds; a gray line shows the corresponding evolution when no neutrinos are taken into account (no M1). Right panel: evolution of the total neutrino luminosity (black solid line) together with the contributions from heavy neutrinos (green dashed line), electron neutrinos (red dashed line), and antineutrinos (blue dashed line).
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: The same as in Figure 4, but when neutrinos are not taken into account; see also Figure 2.
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: The same as Figure 2, but on a smaller scale to highlight features near the HMNS.
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: The same as in Figure 3, but for a GRMHD simulation without neutrino transfer.
Paper: On the Impact of Neutrinos on the Launching of Relativistic Jets from “Magnetars” Produced in Neutron Star Mergers
Authors: Carlo Musolino, Luciano Rezzolla, Elias R. Most
Figure caption: The same as in Figure 2, but for a GRMHD simulation without neutrino transfer. Note that the breakout still takes place but at much later times (t − tmer ≃ 50 ms) and that the steady state (t − tmer ≃ 100 ms) shows weaker, less collimated, and slower outflows. Note the considerably different range in which Ye is shown.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Selected observables from the disk of HD 135344B. Top row: velocity map extracted from the centroid of Gaussian fits to 12CO J = 3−2 line intensity profiles. A zoom-in around the center of the target illustrates the Band 7 continuum emission and the coexistence of dust substructures and velocity perturbations. Bottom panels: selected 12CO intensity channels for the same source, converted to brightness temperature using the Rayleigh–Jeans approximation. In all panels, the background grid follows the 12CO emission surface and the best-fit model orientation retrieved by DISCMINER. For reference, arrows mark the location of example intensity kinks identified in the middle row channels (see also C. Pinte et al. 2025 for a discussion).
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 11 but for the disk of LkCa 15. The 13CO and CS models are assumed to be optically thin and therefore use a “sum” kernel to combine the contributions of the front and back sides to the total intensity (see Sections 3 and 4.1 for details). CS isovelocity contours are shown in yellow to highlight regions where increased intensity results from overlapping column densities of the front and back sides at matching line-of-sight velocities.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Selected 12CO (top), 13CO (middle), and CS (bottom) intensity channels for the disk of HD 135344B. Each panel displays, from top to bottom, the channel maps for the data, the best-fit model, and the corresponding residuals, with residuals below 3 times the rms noise whited out. Peak intensity maps and residuals are shown in the leftmost column of each panel. Solid and dashed lines overlaid on the channel maps represent isovelocity contours from the model’s front and back sides.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison of line width and peak intensity residuals obtained from CS J = 7−6 emission for the disk of LkCa 15 using two models. The first model (top rows) considers only the contribution of the upper surface to the total intensity profile, while the second model (bottom rows) incorporates the summed contribution from both upper and lower emission surfaces. The latter model provides a better reproduction of line width signatures along the disk’s diagonal axes and intensity features along the disk’s main axes, which result in lower line width and intensity residuals as illustrated in the rightmost panels.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison of velocity maps derived from single- and double-component fits applied to the 12CO line profiles of the disk around LkCa 15. Quadratic fit velocity maps show significant back-side contamination, particularly on the near side of the disk, and are susceptible to channelization effects as they consider a limited number of velocity points around the line peak for fitting, reducing their accuracy. Gaussian moments are accurate but exhibit reduced precision near the disk’s diagonal axes due to back-side contamination. Double-component moments are less affected by the back-side contribution, resulting in improved precision in the velocity maps and offering greater accuracy compared to the quadratic method, as they are less influenced by the channel spacing of the datacube. To evaluate the fit quality for the different kernels, the bottom row shows reduced-χ2 values, calculated as ﹩{\chi }_{\nu }^{2}={({n}_{{\rm{ch}}}-{n}_{{\rm{pars}}})}^{-1}{\sum }_{j}^{{n}_{{\rm{ch}}}}{({I}_{d,j}-{I}_{m,j})}^{2}/{s}_{j}^{2}﹩ in the image plane,where sj is a uniform weighting factor defined as the standard deviation of the observed intensity per channel, measured from line-free pixels.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Peak intensity (top), line width (middle), and velocity profiles (bottom) extracted from 12CO J = 3−2 emission for the front side of the disks of HD 135344B and LkCa 15, both imaged with a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15 beam, compared to the best-fit model quantities obtained with DISCMINER. The physical size of the beam’s major axis is shown as a gray Gaussian profile in the top panels. Vertical lines indicate the radial locations of gaps (D) and rings (B) identified in the millimeter continuum by P. Curone et al. (2025). Peak intensities have been converted to brightness temperature units via the Rayleigh–Jeans approximation. Error bars in the top panels and shaded regions in the bottom panels represent the standard deviation divided by the square root of the number of independent beams along each projected annulus. Gray points in the background of the peak intensity and line width profiles represent values extracted from all pixels in the image, mapped into the disk frame.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Selected 12CO J = 3−2 spectra from the disk of LkCa 15 along annuli at R = 200 au (left) and R = 500 au (right), sampled every 30∘ in the disk frame, at the locations marked by numbers in the central panel. The dotted lines in the outer subpanels highlight the systemic velocity of the object. The black solid lines represent the observed spectra, while the orange lines depict the double-bell fits applied to them. Green and magenta shades are also shown within the double-bell fits to illustrate the primary and secondary components of the intensity profile, associated with the front and back sides of the disk, respectively. The background of the subpanels is color coded, with red and blue regions indicating the redshifted and blueshifted zones.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: On-sky orientation of the exoALMA targets, illustrating the model vertical structure of the disks and the projected Keplerian rotation of their front sides as inferred with DISCMINER using fiducial images of the 12CO J = 3−2 line. The window size is adjusted to match the physical extent of each disk, while the beam size, shown in the lower-left corner, remains fixed at 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15. The rotation direction adopted for each disk is noted beside the target names. The outer extent of the modeled back-side structure is also visible when it is sufficiently separated from the front-side outer edge.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Illustrating the two-component fitting process for a region of the LkCa 15 disk where the back-side 12CO emission is prominent and sometimes dominant. Pixels colored in blue and yellow are refitted using new initial guesses, calculated as the median values of parameters from an 11 × 11 grid of neighboring pixels where the fit was otherwise successful (see Section 4.2). After 10 iterations, the majority of the originally flagged and single-component pixels have converged into a double-component fit, with well-distinguished front- and back-side contributions.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Selected 12CO J = 3−2 spectra extracted from the disk of HD 135344B along an annulus at R = 100 au, sampled every 30∘ in the disk frame, at the locations marked by numbers in the central panel, which displays the peak intensity of the disk. The dotted lines in the outer subpanels highlight the systemic velocity of the object. The black solid lines represent the observed spectra, while the orange lines depict the Gaussian fits applied to them. The background of the subpanels is color coded, with red and blue regions indicating the redshifted and blueshifted zones, respectively.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Illustrating Gaussian vs. Bell profiles and their corresponding fits. The profiles are sampled by blue circles every 0.1 km s−1, with an rms noise of 1.4 K, mimicking our fiducial data (see R. Teague et al. 2025). The true amplitude of both profiles is 40 K. The Gaussian width at half-maximum is 0.41 km s−1, which is best fit by a Bell kernel with an amplitude of 38.4  ±  0.9 K, a line width of 0.41  ±  0.01 km s−1, and a line slope of 1.8  ±  0.1. Thus, while the Bell kernel slightly underestimates the Gaussian amplitude, the retrieved width is consistent.