adsabs/AstroCLIMB huggingface dataset:
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Detections of rovibrational bands of water emission in J1605 (top), NC1 (middle), and J1558 (bottom). The continuum-subtracted spectra are shown in black, and the LTE water slab models are shown in blue. The slab model parameters (temperature, column density, and emitting radius) are chosen to roughly match the observed spectra and are not obtained from fits: 525 K, 1020 cm−2, 0.02 au for J1605; 525 K, 1019 cm−2, 0.02 au for NC1; and 525 K, 1018.33 cm−2, 0.03 au for J1558. The red dots show the detected water lines in the least contaminated window.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Simulated molecular emission at short wavelengths (<8 μm). The top panel shows the peak-normalized slab model spectra of several molecules commonly detected in VLMS disks along with the rovibrational band of water at column densities and temperatures of 1018.5 cm−2 and 525 K, respectively. The column densities for CH4 and C2H2 are 1022 cm−2. The black box shows the water-dominant region (6.5–6.8 μm), of which the bottom panel shows a zoom-in, highlighting the least contaminated region to identify the water rovibrational emission in observations. We assume a spectral resolving power of R = 3500.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Stacked spectra of the sources in which pure rotational lines of water are not detected (black); the four panels show the 16–25.5 μm region. The water slab model spectrum is shown in blue, and the gray shaded region around the spectrum shows the ±3σ noise level measured at wavelengths indicated by vertical gray boxes.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Cross-correlation of the observed spectrum of HD 172555 (M. Samland et al. 2025) with water slab models following the same procedure as in Figure 6. The panel on the left shows the cross-correlation with the debris disk spectrum and the water slab spectra, while in the remaining three panels, we have added a synthetic water slab spectrum at 325 K and column density of 1018.5 cm−2 and varying strengths. Here 1×, 3×, and 10 × ﹩{\sigma }_{{{\rm{H}}}_{2}{\rm{O}}}﹩ represent the synthetically added water spectra, each normalized to 1, 3, and 10 times the noise level, respectively.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Thermal gradient in VLMS water emission. The hot water spectra (cyan) are the same as in Figure 3 obtained by a visual fit to the rovibrational band, and the cold water spectra (magenta) are the same as in Figure 4 but scaled to match the flux deficit between the observed spectra (black) and the hot water components. The line positions of the pure rotational lines detected in Figure 4 are also highlighted.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Cross-correlation between synthetic spectra of carbon-bearing molecules with water slab models following the same procedure as in Figure 6. Similar to Figure 21, the panel on the left shows the cross-correlation with the synthetic spectrum and the water slab spectra, while in the remaining three panels, we have added a synthetic water slab spectrum at 325 K and column density of 1018.5 cm−2 and varying strengths.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Same as Figure 4 but in the wavelength range 24–26 μm.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Same as Figure 4 but in the wavelength range 18–20 μm.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Same as Figure 6 but for the rovibrational band emission between 6.55 and 6.70 μm. The contours of the correlation coefficients at −0.5, −0.25, 0, 0.25, 0.5, and 0.75 are shown with dark gray lines. The orange plus sign indicates the best correlation coefficient for sources with a positive correlation.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: The individual synthetic spectra of carbon-bearing molecules that are combined to perform the cross-correlation with water slab spectra in Figure 23. For reference, a synthetic water spectrum at the 1σ level, corresponding to the second panel of Figure 23, is shown in blue.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Same as Figure 4 but in the wavelength range 22–24 μm.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Same as Figure 4 but in the wavelength range 20–22 μm.
Paper: Discovery and Dynamics of the Nontransiting Planet Kepler-139f
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Top: schematic diagram of the Kepler-139 system. The circles representing the planets are spaced logarithmically according to the planets’ semimajor axes, with radii proportional to ﹩\sqrt{{R}_{p}}﹩ (with Rp estimated for planets f and e based on the mass–radius relation of J. Chen & D. Kipping 2017). Bottom left: secular (Laplace–Lagrange) evolution of the Kepler-139 planets’ orbital inclinations, assuming the outer giant is inclined by 3° with respect to the inner system. The gray time ranges are when planets d, b, and c have sufficiently low mutual inclinations to all be observable as transiting planets from a single line of sight (i.e., P(b, c, d transit)  >  0). Bottom right: the time-averaged transit probability for planet f, given that planets d, b, and c transit, as a function of the outer giant’s initial inclination. The dynamical influence of an inclined outer giant lowers the transit probability of planet f by a factor of a few. Dashed lines indicate the transit probability for planet f in the absence of an outer giant.
Paper: Discovery and Dynamics of the Nontransiting Planet Kepler-139f
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: TTVs measured for Kepler-139d (red), Kepler-139b (blue), and Kepler-139c (green). In the top row, the black curves are based on a model fitted to the TTVs and RVs that includes only the four previously known planets. The four-planet model fails to reproduce the 30 minute TTVs of planet c. In the bottom row, the black curves are based on a five-planet model, including a 45 M⊕ nontransiting planet with a period of 354 days, placing it wide of the 2:1 MMR with planet c. The five-planet model provides a far superior fit (﹩{\rm{\Delta }}{\chi }_{{\rm{TTV}}}^{2}\,=\,60﹩).
Paper: Discovery and Dynamics of the Nontransiting Planet Kepler-139f
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: RV data for Kepler-139 (black) from L. M. Weiss et al. (2024). The blue curve is the four-planet model that best fits the RV and TTV data (residual root mean square of 4.4 m s−1). The red curve is the best-fit five-planet model (3.6 m s−1 residual root mean square). The middle panel shows the deviations between the data and the best-fit four-planet model, and the bottom panel shows the same for the five-planet model. The five-planet model provides a significantly better fit to the observed RVs (﹩{\rm{\Delta }}{\chi }_{{\rm{RV}}}^{2}\,=\,77﹩). The gray error bars in the bottom panel show the uncertainties after accounting for the “jitter” term described in Section 4.2.
Paper: Discovery and Dynamics of the Nontransiting Planet Kepler-139f
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Transit light curves of Kepler-139c from Kepler (black) along with the best-fit models (red). Fits were performed using the short-cadence (1 minute) light curves when available, but the data are shown here in 30 minute bins for ease of visualization. The gray dashed line marks the expected transit midpoint if the planet’s period were exactly constant. The data reveal TTVs of up to ∼0.5 hr.
Paper: Cosmological Parameter Estimate from Persistent Radio Sources of Fast Radio Bursts
Authors: Zi-Liang Zhang, 子良 张, Bing Zhang, 冰 张
Figure caption: Observed and simulated PRS population. Main panel: luminosity–redshift distribution for mock (gray/blue) and observed PRSs (orange). The red curve indicates the detection threshold. Upper/right panels: intrinsic redshift distribution Ψ(z) and luminosity function Φ(Lν) (gray), compared to detected mock PRSs (blue).
Paper: Discovery and Dynamics of the Nontransiting Planet Kepler-139f
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Kepler observations of Kepler-139 over time ranges when transits of planet f would be expected. Each panel spans the 90% confidence range of transit times predicted by the five-planet model (Table 1). Transits of planets b and c are highlighted in blue and green. The expected transit signals for planet f, assuming Rp  =  4 R⊕ and b  =  0.5, are shown in orange. Such signals would have been easily detectable but are not seen.
Paper: Cosmological Parameter Estimate from Persistent Radio Sources of Fast Radio Bursts
Authors: Zi-Liang Zhang, 子良 张, Bing Zhang, 冰 张
Figure caption: Posterior distributions from MCMC analyses of Equation (6). The contour plot is smoothed using kernel density estimation. Blue, orange, and green solid lines correspond to fitting results for detected mock PRSs and real PRSs analyzed using the YMW16 model and the NE2001 model, respectively. In each contour set, 1σ, 2σ, and 3σ confidence regions appear from innermost to outermost. Blue dashed lines indicate the median values of the injected distributions of the Monte Carlo simulation.
Paper: Discovery and Dynamics of the Nontransiting Planet Kepler-139f
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Posterior probability densities for the parameters of the five-planet model for Kepler-139, fitted to the TTVs and RVs. Black contours denote the 0.5σ, 1.0σ, 1.5σ, and 2.0σ joint confidence levels, and 1D histograms show the marginalized distributions. To make this figure of manageable size, we omitted the eccentricity parameters and the periods and mean longitudes of the three transiting planets; the median values and uncertainties for those parameters are reported in Table 1.
Paper: Cosmological Parameter Estimate from Persistent Radio Sources of Fast Radio Bursts
Authors: Zi-Liang Zhang, 子良 张, Bing Zhang, 冰 张
Figure caption: Posterior distributions from MCMC analyses of Equation (2). The posterior distribution of ﹩{\rm{lg}}\,{\zeta }_{e}{\gamma }_{{\rm{th}}}^{2}{(R/0.01\,{\rm{pc}})}^{2}﹩ in Figure 2 is adopted as the prior distribution.
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: Mass and radius of TOI-421 b, with mass–radius relations showing the maximum and minimum envelope mass fractions consistent with the planet’s measured properties. Percentages shown are the total envelope mass fractions; the envelope itself consists of ∼99% H/He and 1% H2O by mass, consistent with atmospheric constraints from this study. Earth-like and pure silicate mass–radius relations are shown for comparison. Gray points with error bars show planets with similar masses and radii, taken from the NASA Exoplanet Archive (https://exoplanetarchive.ipac.caltech.edu).
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: Integrated intensities of the CH3OH Eu = 7 K transition (20,2–10,1 A+, shown as green contours), the CH3OH Eu = 20 K transition (20,2–10,1E1, shown as orange contours), and the 3 mm continuum (black rasters). The small ellipse in the bottom left corner represents the synthesized beam. The contour levels for the CH3OH 7 K transition (green) are set at [5σ, 25σ, 45σ, 65σ, 85σ]. The contour levels for the CH3OH 20 K transition (orange) are set at [5σ, 15σ, 25σ].
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 map matrix of G205.46-14.56M3. 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 origins of the coordinates are set at the 3 mm continuum peak position. The velocities labeled on the top and the right are for N2H+ and CH3OH, respectively.
Paper: On the Evidence of a Dark Matter Density Spike around the Primary Black Hole in OJ 287
Authors: Debabrata Deb, Achamveedu Gopakumar, Mauri J. Valtonen
Figure caption: Plots for the variation of the ratio ﹩{\dot{E}}_{{\rm{DF}}}/{\dot{E}}_{{\rm{GW}}}﹩ as a function of γsp while using SMBH binary description of OJ 287 as given in Table 2 of L. Dey et al. (2018). The uncertainty levels associated with the observed 2015 and 2019 impact flares in our model lead to upper bounds marked by the dashed lines, influenced by the approach of M. W. Horbatsch & C. P. Burgess (2012). Both these upper bounds are inconsistent with the estimated value of γsp by M. H. Chan & C. M. Lee (2024).
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: The high angular and spectral resolution of the exoALMA data enables a detailed exploration of the 3D physical and dynamical structure of protoplanetary disks. Panel (a) shows the projection of the inferred emission surface of the 12CO emission from the disk around LkCa 15 shown in panel (b). As described by M. Galloway-Sprietsma et al. (2025), the gray points are individual measurements while the black line shows a moving average with a window of ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩. This deprojection allows for a precise vϕ profile to be extracted, as shown by the orange points in panel (c), which reveals a significant departure from purely Keplerian rotation, as shown by the dotted gray line (J. Stadler et al. 2025). The global profile can be well recovered with a model, shown by the gray line, that includes a radial pressure gradient and the inclusion of the self-gravity of the disk (C. Longarini et al. 2025). The localized variations, most readily discernible in the residuals shown in panel (d), can be associated with localized pressure variations within the disk (J. Stadler et al. 2025).
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: A summary of the exoALMA sample with all sources showing evidence of gas substructures. All images show the 12CO (3–2) peak intensity obtained with bettermoments (R. Teague & D. Foreman-Mackey 2018) using a quadratic fit to the data and masked with the CLEAN masks. Each source has a variable field of view, and the open circle in the lower left of each image denotes the ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩ synthesized beam for reference. The color maps are individually scaled for each source to emphasize the emission morphology rather than for a quantitative comparison (which is provided by M. Galloway-Sprietsma et al. 2025).
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: The high sensitivity of the exoALMA data reveals structures and subtle perturbations previously undetectable. As an example, the channel maps show 12CO emission from the disk around MWC 758, which exhibits significant non-Keplerian components, such as the large arc in the southwest of the disk. C. Pinte et al. (2025) leverage this sensitivity to look for indications of embedded planets in the exoALMA sources. Similarly, the right panel shows the variations in line width of the 12CO emission after subtracting an azimuthally averaged value, revealing a striking spiral morphology. A. F. Izquierdo et al. (2025) describe how such analyses were conducted for the exoALMA sample and how they were characterized. All panels share the same field of view and the ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩ beam is shown in the lower left corner of each.