adsabs/AstroCLIMB huggingface dataset:
Paper: Astrometric Binary Classification via Artificial Neural Networks
Authors: Joe Smith
Figure caption: The architecture of the proposed ANN, where the inputs are the six features associated with the input binary candidate (Section 2.1). See Table 1 for the model architecture of the ANN in detail.
Paper: Astrometric Binary Classification via Artificial Neural Networks
Authors: Joe Smith
Figure caption: ROC curves for each of the comparison models are plotted.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Panchromatic HST and JWST/NIRCam images of the three galaxies with spectroscopically confirmed redshifts z spec. The RGB image shown on the left is made with JWST/NIRCam F150W (B), F182M (G), and F210M (R) images. We use a linear color scale for the RGB cutout to better show the substructures. The pink circle at the bottom-left marks the FWHM of the NIRCam/F210M PSF (Appendix A). Small panels show cutouts of 23 individual filters covering observed λ ≈ 0.35−5μm included in the analysis of this work, where the newly obtained 14-filter NIRCam images are labeled with a hexagon symbol at the bottom right. The last small panel shows the segmentation map. The cutouts of individual filters are shown in a log color scale, highlighting the smooth component of the galaxies.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Similar to Figure 3, but for the remaining three galaxies with photometric redshifts z phot.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Examples of galaxies with different types of substructures identified by our visual selection (see Section 2.1). The RGB cutouts shown here are made with JWST/NIRCam F150W (B), F182M (G), and F210M (R) images. The pink circle marks the angular resolution (FWHM) of NIRCam/F210M imaging. Our visual identifications find a sample of 37 galaxies having substructures with distinct colors at rest-frame 4000 Å. These galaxies show diverse substructures, and can be generally categorized into three groups. The left panel shows an example galaxy with a red, prominent stellar core. The middle panel shows an example galaxy with a dusty core, where in the RGB (made with images at rest-4000 Å) cutout, a flux deficit is seen near the center of the NIRCam/F480M image (rest-1 μm, starlight). The right panel shows an example galaxy with a compact blue center. In this paper, we will only focus on six galaxies having visually identified prominent, red stellar cores at rest-frame 4000 Å (similar to the example galaxy shown in the left panel), while the latter (middle and right) two types of galaxies will be studied in forthcoming papers.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: The parent sample of 3 < z < 4.5 galaxies from JEMS. The x-axis shows the stellar mass from our PROSPECTOR SED fitting (Section 2.4), the y-axis shows the half-light radius derived directly from the F210M surface brightness profile (no point-spread function (PSF)-convolved analysis included). Red circles show the 37 galaxies with visually identified substructures having distinct rest-frame colors at 4000 Å. The golden hexagons show the final sample of six galaxies with red, massive cores presented in this work (see Section 2.1 for the detailed sample selection).
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: Musca. Left: column density map is used to build the radial profile of Musca by sampling radial cuts (red thin lines) with a step of 0.1 pc along the spine (thick red line). The spine is determined by Radfil using the provided mask using the B-spline smoothness algorithm (Zucker & Chen 2018). The radial distance is defined as the projected distance from the considered pixel to the peak emission (blue dot) on a given cut. Right: background fit (upper) and Plummer-like fit (lower). The results of the fit following Equation (10), are shown in the inserts. Green and blue shaded areas are the regions used for the background and Plummer-like fit, respectively.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. Comparison of the polarization degree vs. dust temperature relation from our models (color lines) with observational data (black line). The shaded area represents the 1σ deviation of each bin of data points, which are shown by points (black for observation data and color for model data). The ideal polarization model overestimates the observational data (blue and orange lines), but the realistic polarization model (red line) considering RAT-A, RAT-D, and B-field tangling (﹩{P}_{\mathrm{mod}}﹩) can best reproduce the observed variation of P–T d.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. Comparison of the polarization fraction between our models and observations for different initial maximum sizes of ﹩{a}_{\max }=0.25\,\mu {\rm{m}}﹩ (left panel) and ﹩{a}_{\max }=1\,\mu m﹩ (right panel). The latter realistic models (red line) can reproduce better the data for the region of high density but low temperatures of T d < 50K, revealing the significant grain growth in this dense region.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: Musca: comparison of the polarization degree vs. dust temperature relation from our models (blue line) with observational data (black line). The shaded area represents the 1σ deviation of each bin of data points. The observed increase of P with T d can be successfully reproduced by the polarization model based on the RAT-A theory.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. Same as Figure 8 but for P−N(H2) relation. The ideal polarization model (blue and orange lines) cannot reproduce the data, but the realistic polarization model (red line) considering RAT-A, RAT-D, and B-field tangling (﹩{P}_{\mathrm{mod}}﹩) can best reproduce the observed polarization hole.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. Comparison of the polarization degree vs. dust temperature relation from our models (color lines) with observational data (dashed line). The shaded area represents the 1σ deviation of each bin of data points.
Paper:  B-fields and Dust in Interstellar Filaments Using Dust Polarization (BALLAD-POL). II. Testing the Radiative Torque Paradigm in Musca and OMC-1
Authors: Nguyen Bich Ngoc, Thiem Hoang, Pham Ngoc Diep, Le Ngoc Tram
Figure caption: OMC-1. Comparison of the polarization degree vs. column density relation from our models (color lines) with observational data (dashed line). The shaded area represents the 1σ deviation of each bin of data points.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Left: effects of geometry and offset on the residual continuum maps. The first three columns show the effects of the inclination (inc) and position angle (PA), and the last three columns show the effect of the disk offset with respect to the phase center (ΔR.A., Δdecl.). The central panel highlighted in green is the residual map corresponding to the central values of geometry and offset presented in Figure 3. The isocontour in all panels is taken from Figure 2 at 3σ level. Right: dust continuum clean image. The color bar was adjusted to visualize the high-intensity emission. The solid lines show the disk's minor and major axis, while the solid ellipse shows an ellipse computed from the position angle and disk inclination and centered at the disk offset. The yellow cross shows the disk center computed from the 12CO kinematics. The white dashed lines are the 3σ isocontours from the residual map of the central panels in the green boxes of the left figure.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Top panels from left to right: 12CO (J = 2–1), 13CO (J = 2–1), C18O (J = 2–1), and H2CO (J = 3(0,3)–2(0,2)) moment 0 maps without JvM correction. Middle panels: peak intensity maps for the same molecular lines without JvM correction. Bottom-left panel: Dust continuum emission map with a Briggs robust parameter = 0.5 and an additional faint source detection. Contour levels are 4σ in this panel. Bottom-right panels: 12CO emission channel maps at 4.2 and 4.3 km s−1 without JvM correction. Dust continuum isocontours at 3σ from Figure 2 are shown in all panels with molecular line data.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Maps in the top-left panels: different estimation of the line-of-sight velocity. From left to right: first Moment, Quadratic, Gaussian, GaussThick. Maps in the bottom-left panels: Residuals after subtracting the best-fit model of each velocity map. Right panels: Molecular line spectrum at two pixels within the green circle of the left panels. The vertical lines are the line-of-sight velocities estimated from the Gaussian (solid line) and quadratic (dashed line) methodologies. The spectral resolution is shown as a horizontal line in the top panel.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Additional channel maps of the 12CO emission around J16120. The color bar on the right is the same for all panels. The synthesized beam is shown in the bottom-left panels, and a horizontal line with a size of 100 au is shown in the last row and first column panel.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Estimated total dust mass for different disk-averaged maximum grain size models. The horizontal dashed line shows the estimated dust mass in L. Trapman et al. 2024, in preparation. The vertical shaded area represents the ﹩{a}_{\max }﹩ constraint estimated from the spectral index for a particle size distribution ranging from p = 2.5 to 3.5.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Kinematic modeling of CO (first column), 13CO (second column), C18O (third column), and H2CO (fourth column). The first row shows the velocity field maps, the second row is the best-fit velocity model, and the third row is the velocity residuals.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Fraction of CPD fluxes that are recovered as a function of the CPD input flux within the gap of J16120. The 50% recovery fraction (horizontal dotted line) corresponds to 93 μJy (vertical dotted line).
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Corner plots of the last 3000 steps of the Markov Chain Monte Carlo used to explore the 12CO emission surface parameters.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Dust continuum modeling of the disk around J16120. Top-left panel: observed binned visibilities (blue and orange dots, at a bin size of 103 and 104 λ, respectively), and visibility model (black curve) of the dust continuum data. Top-right panel: Deprojected continuum radial profile from the image plane (blue curve) and from the visibility fit nonconvolved model (orange curve). The arrow marks the radial position of the compact emission. Bottom-left panel: CLEAN image of the dust continuum data. Bottom middle panel: CLEAN image of the visibility model. Bottom right panel: CLEAN image of the visibility residuals. The isocontour in the bottom panels is at a 3σ level.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Gas kinematics inferred from the 12CO channel maps in the disk around J16120. Solid blue lines in the top panels show the azimuthal, radial, and vertical velocity (from left to right) as a function of radius. Error bars are 1σ uncertainties, and the vertical bar in the middle and right panel shows the spectral resolution of the data. The orange line in the top-left panel is the Keplerian model in the midplane. The embedded plot in the top-left panel zooms in on the radial profiles around the dust ring. Bottom left: normalized deviation of the azimuthal velocity with respect to the Keplerian model (blue line) and expected velocity deviation of an unperturbed smooth disk (green shaded area). Bottom middle: velocity field in the radius–height plane. The blue line is the parameterized 12CO emission surface. Bottom right: velocity field in the radius–azimuth plane. The color bar shows the deviation of the azimuthal velocity with respect to the Keplerian model. The error bars of the velocity vectors in each direction can be seen in the radial profile panels. In all panels, the continuum radial profile is shown as a dashed gray line for reference.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Spiral arm structure inferred from the disk azimuthal asymmetries. Left panel: zoom into the residual map in Figure 2. Black markers are the position of the spiral arm structure, the green solid line is the best-fit spiral model, and its extrapolation is shown as a green dashed line. The purple lines around the red knots are 3σ isocontours. The blue lines at 0° and 90° are the disk's major and minor axis, respectively. Right panel: azimuthal position and deprojected radius of the spiral arm structure (black markers), and best-fit model (green solid line). The thin turquoise solid lines represent 1000 random chains from the posterior distribution.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Continuum and molecular emission of the disk around J16120. First row: dust continuum map (left) and dust continuum radial profile (right). Second row from left to right: 12CO (J = 2−1), 13CO (J = 2−1), C18O (J = 2−1), and H2CO (J = 3(0,3)−2(0,2)) moment 0 maps and azimuthally average radial profiles. Third row: peak intensity maps for the molecular lines in the above panels in addition to the continuum radial profile. Fourth row: moment 1 maps for the molecular lines in the above panels and velocity along the disk major axis. The beam is shown as a dashed ellipse in the bottom-left corner of each panel, and in the bottom-left corner of the moment 0 map radial profile panel. Dust continuum isocontour at 3σ is shown in all panels.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption:  12CO velocity modeling of the disk around J16120. Left: observed velocity structure in 12CO. Middle: best-fit Keplerian model. Emission contours corresponding to 4σ, 8σ, and 12σ of the 4.2 km s−1 channel map (Figure 4) are included as a spatial reference. Right: velocity residuals. The green circle highlights a velocity structure at the position of the kinematic perturbation shown in Figure 4.