adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of a Radio Megahalo in the Cluster PLCKG287.0+32.9 Using the uGMRT
Authors: Sameer Salunkhe, Ramananda Santra, Ruta Kale
Figure caption: Top left: uGMRT band 3 high-resolution image (﹩10\mathop{.}\limits^{^{\prime\prime} }5﹩ × ﹩9\mathop{.}\limits^{^{\prime\prime} }8﹩, PA: ﹩9\mathop{.}\limits^{^\circ }3﹩ and σrms = 35 μJy beam−1). Top right: uGMRT band 4 high-resolution image (10﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 × 9﹩\mathop{.}\limits^{\unicode{x02033}}﹩6, PA: ﹩25\mathop{.}\limits^{^\circ }9﹩, σrms = 25 μJy beam−1). Previously observed radio sources are labeled here. Bottom left: uGMRT band 3 low-resolution image (﹩27\mathop{.}\limits^{^{\prime\prime} }3﹩ × ﹩19\mathop{.}\limits^{^{\prime\prime} }4﹩, PA: ﹩33\mathop{.}\limits^{^\circ }1﹩, σrms = 60 μJy beam−1). Bottom right: uGMRT band 4 low-resolution image (﹩27\mathop{.}\limits^{^{\prime\prime} }8﹩ × ﹩17\mathop{.}\limits^{^{\prime\prime} }5﹩, PA: ﹩27\mathop{.}\limits^{^\circ }2﹩, σrms = 45 μJy beam−1). Contour levels for all images are drawn at [±1, 2, 4, 8, . . . ] × 3σrms, where σrms is the rms noise of the respective image. The red ellipse in the bottom left corner of each panel indicates the beam size of the image in the respective panel.
Paper: Observations of 1/f Noise at Mercury’s Solar Wind Using MESSENGER Data
Authors: Rayta A. Pradata, Sohom Roy, William H. Matthaeus, Jiaming Wang, Rohit Chhiber, Francesco Pecora, Yan Yang
Figure caption: (a) Measurements from MESSENGER’s Magnetometer during Day 34 of 2013, along with the solar wind selections. The panels from top to bottom show the radial, tangential, and normal components as well as the magnitude (BMAG). (b) Selected and concatenated solar wind magnetic field intervals as observed by MESSENGER during the entire year 2013, in RTN components and magnitude. (c) Smaller fraction of the concatenated time series (only showing BMAG), at ≈2 days, to show the abundance of gaps in the data set.
Paper: Discovery of a Radio Megahalo in the Cluster PLCKG287.0+32.9 Using the uGMRT
Authors: Sameer Salunkhe, Ramananda Santra, Ruta Kale
Figure caption: DSS2 i-band optical image overlaid with uGMRT band 3 (σrms = 60 μJy beam−1, where beam = 30″ × 30″) in violet and band 4 (σrms = 20 μJy beam−1, where beam =  ﹩8\mathop{.}\limits^{^{\prime\prime} }9\times 7\mathop{.}\limits^{^{\prime\prime} }8﹩) in red raster. The yellow dashed circle indicates the R500 of the cluster.
Paper: Observations of 1/f Noise at Mercury’s Solar Wind Using MESSENGER Data
Authors: Rayta A. Pradata, Sohom Roy, William H. Matthaeus, Jiaming Wang, Rohit Chhiber, Francesco Pecora, Yan Yang
Figure caption: (a) Magnetic field spectrum S(f) of the superposed solar wind time series during 2013, with τc = 45101  s and μc = 1206 s, computed with the Blackman–Tukey method. The reciprocal frequencies are marked in the figure, along with the −1 and −5/3 reference slopes. (b) The same as (a), but plotted as a compensated spectrum fS(f). A 1/f spectrum is indicated by a flat (horizontal) compensated spectrum.
Paper: Observations of 1/f Noise at Mercury’s Solar Wind Using MESSENGER Data
Authors: Rayta A. Pradata, Sohom Roy, William H. Matthaeus, Jiaming Wang, Rohit Chhiber, Francesco Pecora, Yan Yang
Figure caption: (a) Distribution of solar wind interval lengths (in minutes) observed by MESSENGER in 2013, ranging from 53 to 395 minutes. (b) Distribution of gap lengths (lengths of excluded data sets) between solar wind intervals observed by MESSENGER in 2013, ranging from 1.5 to 43.3 hr (excluded from the histogram).
Paper: Observations of 1/f Noise at Mercury’s Solar Wind Using MESSENGER Data
Authors: Rayta A. Pradata, Sohom Roy, William H. Matthaeus, Jiaming Wang, Rohit Chhiber, Francesco Pecora, Yan Yang
Figure caption: Magnetic field spectrum S(f) versus frequency f of a sample solar wind interval during Day 34 of 2013, with correlation time τc = 790 s. The frequency 1/τc = 1.3 × 10−3 Hz is marked by the gray dashed line. The reference −5/3 slope is also shown. The solid line is the boxcar filtered spectrum, employing variable width averaging for clarity.
Paper: Observations of 1/f Noise at Mercury’s Solar Wind Using MESSENGER Data
Authors: Rayta A. Pradata, Sohom Roy, William H. Matthaeus, Jiaming Wang, Rohit Chhiber, Francesco Pecora, Yan Yang
Figure caption: Distribution of correlation times (in minutes) for MESSENGER solar wind intervals near Mercury in 2013. These range from 3 to 78 minutes, from total solar wind data duration of 186 days and 117 minutes. The computed mean correlation time μc is 20.1 minutes.
Paper: Discovery of a Radio Megahalo in the Cluster PLCKG287.0+32.9 Using the uGMRT
Authors: Sameer Salunkhe, Ramananda Santra, Ruta Kale
Figure caption: The surface brightness radial profile is shown, measured on the elliptical annular regions (inset images). The purple and red colors represent the profiles for only the southern diffuse emission to the NW relic in bands 3 and 4, respectively. The teal and orange colors represent the profiles considering both northern and southern diffuse emissions to the NW relic in bands 3 and 4, respectively. The solid line is the exponential fit for the radio halo data. The dashed line marks the detection limit at 1σ for each annulus, and the vertical dotted line shows the cluster’s R500. The annotated figures show the central diffuse emission in uGMRT bands 3 and 4, having a resolution of 40″ and rms values of 120 and 67 μJy beam−1, respectively. Contours are the same as given in Figure 3. The region below 1.5σrms is masked while producing the surface brightness profile.
Paper: Discovery of a Radio Megahalo in the Cluster PLCKG287.0+32.9 Using the uGMRT
Authors: Sameer Salunkhe, Ramananda Santra, Ruta Kale
Figure caption: Left: spectral index map for the radio halo in PLCKG287 at 30″ is shown between 400 and 700 MHz. The black contours are drawn at 3σrms × [1,2,4,8...] from the 400 MHz image. The corresponding error map is shown in the inset, and at the central region, overall the errors are <0.2. Right: the radial profile of the spectral index is shown in this panel. The outer component has a significantly steeper spectrum compared to the radio halo. The annular region used to get the spectral profile is shown in magenta color in the inset, and masked areas are shown with green regions.
Paper: Discovery of a Radio Megahalo in the Cluster PLCKG287.0+32.9 Using the uGMRT
Authors: Sameer Salunkhe, Ramananda Santra, Ruta Kale
Figure caption: Chandra image (in color) of PLCKG287 is shown here. The contours at [1, 3, 9, 27...] × 3σrms from 40″ resolution images of uGMRT band 3 (σrms = 120 μJy beam−1) and band 4 (σrms = 67 μJy beam−1) are added in blue and magenta, respectively. The black “×” sign indicates the peak of the X-ray emission and the black dashed circle indicates the R500 of the cluster.
Paper: Polytropic Behavior in Corotating Interaction Regions: Evidence of Alfvénic Heating
Authors: M. A. Dayeh, M. J. Starkey, G. Livadiotis, S. T. Hart, A. A. Shmies, R. C. Allen, R. Bučik, H. A. Elliott
Figure caption: ((a) Step 1) Solar wind speed (red) and proton density (blue) for an 18 minute period within the uncompressed FSW region of Event 33. ((b) Step 2) Values of the Bernoulli integral for the corresponding data shown in (a). In both (a) and (b), the shaded interval illustrates a single 5-point interval over which the stability condition for the Bernoulli integral must be met. ((c) Step 3) Logarithmic plot of T vs. n fit to a linear model (black line), from which ﹩{\gamma }﹩ is inferred. ((d) Step 4; left) 2D histogram of the normalized number of the derived ﹩{\gamma }﹩ (count percentage) as a function of the solar wind speed. ((d) Step 4; right) 1D histogram of the derived ﹩{\gamma }﹩.
Paper: Polytropic Behavior in Corotating Interaction Regions: Evidence of Alfvénic Heating
Authors: M. A. Dayeh, M. J. Starkey, G. Livadiotis, S. T. Hart, A. A. Shmies, R. C. Allen, R. Bučik, H. A. Elliott
Figure caption: (a) Solar wind speed (black) and magnetic field strength (red) corresponding to Event 2 (1995 January 27) from the catalog used (T. W. Broiles et al. 2012). (b) Solar wind proton density. The four boundaries are indicated at the bottom of the plot and the corresponding regions of the CIR are indicated by color.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Perturbed density (normalized by the initial density) δρ/ρinit at (top panels) Z/R = 0.3 (three scale heights above the midplane at R = 1), (middle panels) Z/R = 0.1 (one scale height above the midplane at R = 1), and (bottom panels) midplane. From left to right, results with FARGO3D, Idefix, Athena++, PLUTO, and Phantom. At high altitudes, Phantom results appear noisy because of the small number of SPH particles in the low-density regions.
Paper: Polytropic Behavior in Corotating Interaction Regions: Evidence of Alfvénic Heating
Authors: M. A. Dayeh, M. J. Starkey, G. Livadiotis, S. T. Hart, A. A. Shmies, R. C. Allen, R. Bučik, H. A. Elliott
Figure caption: (a) Correlation of δB vs. δV in the XGSE direction in Event 2 for the four CIR subregions. (b) Distributions of the correlation coefficients determined for all CIR events using analysis similar to that in panel (a).
Paper: Polytropic Behavior in Corotating Interaction Regions: Evidence of Alfvénic Heating
Authors: M. A. Dayeh, M. J. Starkey, G. Livadiotis, S. T. Hart, A. A. Shmies, R. C. Allen, R. Bučik, H. A. Elliott
Figure caption: (a) Histograms of the average polytropic index for all events and each region of the CIR. Thick black lines indicate the enriched histograms used to calculate the mean value of ﹩\gamma ﹩. (b) Mean value of ﹩{\gamma }_{{avg}}﹩ from the enriched histograms in (a) corresponding to different CIR regions.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 1, but for the meridional velocity vθ.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 1, but for the radial velocity vr.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 1, but for the perturbed azimuthal velocity δvϕ ≡ vϕ − vϕ,init, normalized by the initial azimuthal velocity vϕ,init.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as in Figure 1 but with a linear stretch in the color scale to highlight the changes in intensity within the brightest regions.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 3 but for J1842 and J1852.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 3 but for HD 143006 and HD 34282.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 3 but for DM Tau and HD 135344B.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Real and imaginary parts of the recentered and deprojected visibilities azimuthally averaged into 15 kλ wide bins on an asinh scale as a function of the deprojected baseline length for the data (gray points) and the best-fit models from galario (blue line) and frank (red line). Note that the imaginary part is fitted only when employing a 2D nonaxisymmetric galario model (i.e., for CQ Tau, HD 135344B, HD 143006, HD 34282, and MWC 758), while the imaginary components of the frank and 1D galario axisymmetric models are null for all spatial frequencies by definition.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 3 but for V4046 Sgr.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 3 but for LkCa 15 and MWC 758.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 3 but for J1604 and J1615.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 3 but for PDS 66 and SY Cha.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Stellar mass from discminer (A. F. Izquierdo et al. 2025) and dust disk mass, calculated in Section 2, as functions of the NAI. The uncertainties in stellar mass are too small to be shown, while for the dust disk mass, we show the 10% absolute flux calibration error, which dominates over the statistical uncertainty.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Gallery of CLEAN residuals of the full FOV after deconvolution using a central spherical mask 3″ wide and a 2σ stopping threshold. Each panel shares the same color bar ranging from −0.05 to 0.15 mJy beam−1. The robust value of 2.0 has been employed, and the associated beam is indicated by the black ellipse in the lower left corner of each panel.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as the left panel in Figure 5 but without normalizing the mass accretion rate for its dependence on stellar mass.