adsabs/AstroCLIMB huggingface dataset:
Paper: Toward Accurate Asteroseismic Masses for Luminous Giants
Authors: Kaili Cao, 开力 曹, Marc H. Pinsonneault
Figure caption: A comparison between different correction schemes for asteroseismic masses. All quantities are plotted as functions of ﹩{\nu }_{{\rm{\max }}}﹩, with the lower RGB shown on the left and the upper RGB shown on the right. The upper panel shows the published fΔν from APOKASC-3 for our sample. In the middle panel, we plot the ratio between the adjusted (see text) fΔν and the raw fΔν. In the lower panel, we illustrate the net effect on the masses relative to the published APOKASC-3 values, which correspond to unity and are shown by the blue dashed line. The raw fR correction, holding fΔν fixed (so that the mass correction factor is simply 1/fR), is shown by the green dashed–dotted line. The adjusted fR correction, including feedback in the fΔν calculation, is shown by colored dots. Although it depends on both ﹩{\nu }_{{\rm{\max }}}﹩ and Mseis, simple fitting results using Equation (3) (ignoring mass dependence) are also shown by the orange solid curve. The fitting coefficients are tabulated in Table 1.
Paper: Toward Accurate Asteroseismic Masses for Luminous Giants
Authors: Kaili Cao, 开力 曹, Marc H. Pinsonneault
Figure caption: Impact on FDU predictions for the α-poor population. Each panel plots the difference between two versions of surface carbon-to-nitrogen abundance ratio changes Δ[C/N] (current minus birth) as a function of logarithmic seismic gravity. Upper panel: difference between post-FDU Δ[C/N] values predicted for corrected (adjusted fR correction; “New”) and APOKASC-3 (“Old”) asteroseismic masses. Note that the color-coding has been switched to corrected Mseis. Lower panel: rolling medians of discrepancies between observed (with birth trends removed following J. D. Roberts et al. 2024) and predicted Δ[C/N]; vertical error bars (shaded regions) are MADs multiplied by k ≈ 1.4826. The median trends using APOKASC-3 and corrected masses are shown as blue dashed and orange solid curves, respectively. In both panels, the end of FDU and the center of the RGB bump are shown as green and brown bands, respectively. For both quantities, we use benchmark predictions from K. Cao & M. Pinsonneault (2025); for the latter, we superimpose an observed zero-point shift of 0.1509 dex (see Section 5.2 of K. Cao & M. Pinsonneault 2025).
Paper: Toward Accurate Asteroseismic Masses for Luminous Giants
Authors: Kaili Cao, 开力 曹, Marc H. Pinsonneault
Figure caption: Consistency between lower RGB and upper RGB within the α-rich population. The two columns study the consistency of asteroseismic masses and ages, respectively. The four rows correspond to four correction schemes; from top to bottom: APOKASC-3 without ﹩{\nu }_{{\rm{\max }}}﹩ correction, APOKASC-3 correction, raw fR correction, and adjusted fR correction. In each panel, we compare three combinations of models and weighting approaches: GARSTEC+Mosser (blue solid curves), GARSTEC+White (orange dashed curves), and Sharma+White (green dashed–dotted curves). Rolling medians of masses and ages are shown as functions of ﹩{\nu }_{{\rm{\max }}}﹩; horizontal error bars (shaded regions) are median absolute deviations (MADs) multiplied by k = 1/(Φ−1(3/4)) ≈ 1.4826, which converts MADs to standard deviations for normal distributions (Φ is the cumulative distribution function); overall medians are shown as vertical straight lines. For GARSTEC+Mosser, median masses and ages are tabulated in Table 2.
Paper: Toward Accurate Asteroseismic Masses for Luminous Giants
Authors: Kaili Cao, 开力 曹, Marc H. Pinsonneault
Figure caption: Scatter plots of asteroseismic age τseis vs. frequency of the maximum power ﹩{\nu }_{{\rm{\max }}}﹩. The 4439 “Gold” sample stars are shown in blue, while the 1097 “Silver” sample stars are shown in orange. The two columns present the α-rich and α-poor populations. The first two rows correspond to ages from APOKASC-3 (M. H. Pinsonneault et al. 2025) and our adjusted fR correction, respectively, and the last row shows the ratios between these two sets of age predictions. The age of the Universe (∼13.8 Gyr) is shown as green dashed horizontal lines in the first two rows. All ages shown in this figure are based on GARSTEC (A. Weiss & H. Schlattl 2008) models and the B. Mosser et al. (2012) weighting approach.
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: Schematic of current/density sheets considered in this work. Left: overdense current sheet with density perturbation Δne kept in pressure balance by a folded magnetic field. For layers of multiple current sheets, as often seen in simulations of large-amplitude MHD turbulence, there are both overdense and underdense sheets. Middle: significant radio-wave scattering, i.e., an ESE, occurs when the sheet is aligned favorably for the light ray to traverse a large column density parallel to the sheet. Right: the folded field lines are responsible for strong CR scattering, which occurs at the end of the sheet when particles experience resonant field-line curvature. We discuss alternative sheet geometries in Appendix B.
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: The lensing behavior of an aligned sheet. (a) When the source is close to the direction of the sheet, the observer can receive the light bent by the sheet, as well as unlensed light from the LOS, and hence observe magnification of the source. This regime is labeled “a” in the rightmost panel. The dashed line with arrow is the fiducial fixed sky direction, relative to which the source angular position β is defined. The largest bending angle introduced by the sheet sets the size of the angular region on the source plane affected by the lens, which can be used to estimate the occurrence fraction of ESEs. (b) When the source is behind the aligned sheet, the LOS light is bent away, and the observer only sees the faint lensed images and hence observes demagnification of the source. The demagnified region (labeled “b” in the rightmost panel) is determined by the thickness of the sheet and is almost achromatic. (c) In the top panel, the angular profile of the column density projected on the sky can be approximated by a Gaussian with angular width σ approximately equal to half its physical width along the sheet normal, divided by the distance to the sheet. In the bottom panel, the magnification (background color; darker means higher magnification) is a function of angular source position β. The source will be lensed in the region between ±βfocal (Equations (15) and (A6)) and demagnified between ±βdemag (Equations (18) and (A5)). The red and blue dashed lines are analytical approximations of ±βfocal and ±βdemag, which are used to estimate ESE occurrence fraction and sheet thicknesses, respectively.
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: Occurrence fraction of radio sources being lensed by aligned plasma sheets of thickness ∼1 au calculated from Equation (16) in three different frequency bands as a function of the ∼GeV CR mean free path. We assume that the long axis of the sheets ℓ and volume-filling factor fV are constrained by the CR mean free path, λCR ∼ ℓ/fV. For a fixed λCR, Wsrc is then independent of ℓ. The green shaded region shows the rough occurrence fraction of quasar ESEs, with the green dashed line representing the rate ≈0.007 at 2.7 GHz reported in R. L. Fiedler et al. (1987) and R. Fiedler et al. (1994). The gray shaded region shows the predicted approximate occurrence fraction of pulsar ESEs observed at lower frequencies as a function of λCR. Assuming that CR scattering and ESEs are caused by the same density/magnetic sheets of thickness ∼1 au and with Δne ∼ 0.03 cm−3, a CR mean free path of order 10 pc is consistent with the observed occurrence fraction of quasar ESEs (observed at frequencies >1 GHz).
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: ESE behaviors for short-duration radio transients. Large bending angles of the lensed images induce significant time delays, enabling separation by arrival time. This allows the study of lensing structures by tracking the temporal and spectral evolution of individual images, rather than relying on the total flux as done for quasars. Left: the total flux variation summed from all images, similar to Figure 4. Panel (a): variation of brightness (gray scale) and time delay between different images over time as the source moves, sampled at the frequency indicated by the red horizontal dashed line in the left panel. Panel (b): brightness of the images (gray scale) as a function of frequency and delay, measured at the position of the blue vertical dashed line in the left panel. This figure is generated assuming the Gaussian overdense lens described in Appendix A with κ = 10(ν/3 GHz)−2.
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: A schematic light curve of a typical ESE. The two panels show examples of a source with an angular diameter of 1 mas and angular velocity of 0.1 mas day−1 passing through overdense lenses with convergence values of κ = 5 and κ = 20 (Equations (12) and (13)), respectively.
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: Slices of in-plane gradients of column density and integrated magnetic pressure (arbitrary units) from a 10243 subsonically driven simulation of MHD turbulence with a weak guide magnetic field (δB/B0 ≈ 4) taken from P. Kempski et al. (2023). The most intense density sheets, which produce strong radio-wave scattering, are also sheets of strongly varying magnetic field strength, qualitatively consistent with the picture of pressure-balanced current sheets (Equation (2) and Figure 2). Between the two slices, we show the 3D morphology of the turbulence using a sample of highly tangled magnetic field lines, characterized by numerous kinks and reversals that scatter CRs (P. Kempski et al. 2023; M. Lemoine 2023).
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: The Einstein ring of a gravitationally lensed quasar can serve as a probe of interstellar density sheets. In the presence of a sheet characterized by a large aspect ratio, two widely separated regions on the ring can simultaneously undergo an ESE. Such ESE pairs can be identified through synchronized variations in their temporal evolution.
Paper: High Resolution ALMA Data of the Fomalhaut Debris Disk Confirms Apsidal Width Variation
Authors: Jay S. Chittidi, Meredith A. MacGregor, Joshua Bennett Lovell, Gaspard Duchene, Mark Wyatt, Olja Panic, Paul Kalas, Margaret Pan, A. Meredith Hughes, David J. Wilner, Grant M. Kennedy, Luca Matrà, Michael P. Fitzgerald, Kate Y. L. Su
Figure caption: Top left: A mosaic of the Cycle 5 (C5) long-baseline data. The data were imaged to the 5% gain level to highlight the detection of the star, which sits at the edge of the primary beam between the NW and SE ansae pointings. The naturally-weighted beam size is ﹩0\mathop{.}\limits{^{\prime\prime} }50\times 0\mathop{.}\limits{^{\prime\prime} }39﹩ (indicated by the ellipse in the lower left corner of each panel) and the rms noise near the pointing centers is 7 μJy bm−1. The axes are the stellocentric offset in arcseconds and the image is north-aligned. Top right: A mosaic of the NW and SE ansae pointings using the coaligned shorter-baseline Cycle 3 (C3) data as well as the longer baseline C5 data. The naturally-weighted beam size is slightly larger, 0﹩\mathop{.}\limits{^{\prime\prime} }57\times 0\mathop{.}\limits{^{\prime\prime} }44﹩, and the rms is also 7 μJy bm−1. Bottom left: A mosaic of all seven pointings of ALMA Band 6 observations from C2, C3, and C5. The naturally-weighted beam size is ﹩1\mathop{.}\limits{^{\prime\prime} }09\times 0\mathop{.}\limits{^{\prime\prime} }81﹩ and the rms noise near the pointing centers at the ansae is 7 μJy bm−1, but decreases to 12 μJy bm−1 toward the IB (denoted by the dashed white curves, see Section 5.2). The lack of long-baseline observations at the intermediate pointings leads to a beam size that is larger than the naturally-weighted beam corresponding to just the NW and SE ansae data, as in the top right. Bottom right: JWST 25.5 μm image from A. Gáspár et al. (2023) with overlaid contours from the bottom right ALMA mosaic corresponding to the 10σ, 20σ, and 30σ flux levels. This image has been scaled to highlight the intermediate and inner disks, and the positions of the contours have been corrected for the proper motion between the two imaged epochs. The fainter dashed curves denote the IB boundaries as in the bottom left.
Paper: High Resolution ALMA Data of the Fomalhaut Debris Disk Confirms Apsidal Width Variation
Authors: Jay S. Chittidi, Meredith A. MacGregor, Joshua Bennett Lovell, Gaspard Duchene, Mark Wyatt, Olja Panic, Paul Kalas, Margaret Pan, A. Meredith Hughes, David J. Wilner, Grant M. Kennedy, Luca Matrà, Michael P. Fitzgerald, Kate Y. L. Su
Figure caption: First row: A deprojected map of the circumstellar radius vs. azimuthal angle of the Fomalhaut outer disk produced using the mosaic in Figure 1(b). The angular coordinates are with respect to the disk position angle of 335﹩\mathop{.}\limits^{\unicode{x000b0}}﹩84. Second row: A radius vs. azimuth map for the best-fit model without a dispersion in eccentricity, after imaging with CASA. Third row: Same as the second, but for the best-fit model with a dispersion in eccentricity. Fourth row: A radius vs. azimuth map of the 25.5 μm JWST image of the disk. Unlike the ALMA images, the NW ansa is significantly dimmer than the SE ansa. Fifth row: Radial profiles produced using 10° radial cuts centered at 0° (SE ansa near apocenter, red) and 180° (NW ansa near apocenter, yellow) from the above maps. For the ALMA data, the 21% ± 1% brightness asymmetry between the ansae is strongly apparent. The labeled shaded regions are the measured FWHM of the data. “Shoulders” of emission at 20 au interior and exterior to the peak flux in the SE ansa profile and exterior to NW ansa profile are denoted by the colored arrows. The radius of peak emission differ between the data and the models, which is discussed in the text.
Paper: High Resolution ALMA Data of the Fomalhaut Debris Disk Confirms Apsidal Width Variation
Authors: Jay S. Chittidi, Meredith A. MacGregor, Joshua Bennett Lovell, Gaspard Duchene, Mark Wyatt, Olja Panic, Paul Kalas, Margaret Pan, A. Meredith Hughes, David J. Wilner, Grant M. Kennedy, Luca Matrà, Michael P. Fitzgerald, Kate Y. L. Su
Figure caption: Left: A Moment-0 image of the GDC obtained by integrating between 230.1 and 230.4 GHz (173–563 km s−1 channels relative to the expected CO line) of the Cycle 3 residual measurement set (i.e., the best-fit disk continuum model has been subtracted off). The cyan circle denotes the area of the region used to extract the spectrum of the source, and the orange-dashed circle is denotes a region of equivalent size with characteristic noise. Right: The resulting extracted spectra of the background galaxy and noise region. The source emission is redshifted by >400 km s−1 from the expected Doppler-shifted transition of 12CO J = 2–1 corresponding to Fomalhaut (vr = 6.5 km s−1, G. A. Gontcharov 2006), suggesting the source is unaffiliated with the system. The width of the emission is ≈300 km s−1, consistent with velocity dispersion from rotating disk galaxies.
Paper: High Resolution ALMA Data of the Fomalhaut Debris Disk Confirms Apsidal Width Variation
Authors: Jay S. Chittidi, Meredith A. MacGregor, Joshua Bennett Lovell, Gaspard Duchene, Mark Wyatt, Olja Panic, Paul Kalas, Margaret Pan, A. Meredith Hughes, David J. Wilner, Grant M. Kennedy, Luca Matrà, Michael P. Fitzgerald, Kate Y. L. Su
Figure caption: Top row: Apocenter and pericenter plots of the best-fit eccentric disk models without (first column) and with (second column) a free parameter describing a Gaussian dispersion in the proper eccentricity for the particles (see Table 2). These images are full-resolution, i.e., not convolved with the synthesized beam, in order to highlight the underlying differences in intensity. Bottom row: Residual between the data and model with contours highlighting −10σ, −5σ, 5σ, and 10σ noise level. These were imaged with tclean with the same parameters as in Figure 1(c). The ellipses indicate the size of the ALMA beam.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Residual brightness temperature of 12CO after subtracting an axisymmetric power law as observed in MWC 758 (left) and our warped disk model at an estimated CO emission height (middle) and midplane from the model (right). The temperature quoted in each case is the difference from a fitted radial axisymmetric power-law model. The model has been smoothed over a circular beam for visualization purposes, assuming zero temperature residual outside of the simulated range. The CO surface temperature from the model (middle) broadly matches the observed structure (left), but the midplane pattern (right) resembles the m = 2 symmetry in the inner region.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: The total K-band polarized intensity map of MWC 758 (left; B. B. Ren et al. 2023) compared to the total intensity at 2.2 μm from our RADMC3D model (right). Both are masked inside 100 mas, which is the size of the coronagraph. The contours of the right panel are 5σ, 10σ, 20σ, and 50σ from the observed structure. We highlight that we do not have good constraints on warp structure inside of 150 mas, where we have assumed a profile with comparable amplitude to the warp farther out (see Appendix B).
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Visualization of the warp structure via concentric rings with the profile for MWC 758 shown in Figure 1. The coordinate system is chosen such that the disk lies in the x–y plane on average, and the z-axis is stretched by a factor four to emphasize the warp. The disk is then viewed slightly from above.
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: Magnitude of the in-plane gradient of the logarithm of projected column density (with normalization factor ﹩{ \mathcal C }=L{N}_{e0}/\delta {N}_{e,{\mathrm{rms}}}﹩, where L is the turbulence driving scale and Ne0 and δNe,rms are the mean projected column density and rms value of the fluctuating projected column density, respectively) in two high-resolution (22403) subsonic MHD dynamo simulations from A. K. Galishnikova et al. (2022). Blue denotes regions where the local column density Ne is less than the mean column density Ne0, while red and yellow regions correspond to locally enhanced column density. The simulation shown in the left panel was run with Pm = 1 (smaller viscosity), while the simulation shown in the right panel was run with Pm = 100 (larger viscosity). Both simulations use the same resistivity. Notably, in both panels, we see that regions of large column density gradients are highly intermittent and that there are numerous sheets that are remarkably straight. The Pm = 1 case is characterized by contributions from sheets with shorter long-axis lengths with projected gradients that are less extreme relative to the Pm = 100 case (we saturate the color bar, which is shared between the two panels, at ±200 to make structures in the left panel visible), demonstrating that how turbulence is dissipated has significant implications for the geometry of density sheets and thus the occurrence of ESEs.
Paper: A Unified Model of Cosmic-Ray Propagation and Radio Extreme Scattering Events from Intermittent Interstellar Structures
Authors: Philipp Kempski, Dongzi Li, Drummond B. Fielding, Eliot Quataert, E. Sterl Phinney, Matthew W. Kunz, Dylan L. Jow, Alexander A. Philippov
Figure caption: The duration of an ESE depends on the angle ϕ at which the source crosses the sheet. Left: the magnification of the source at different locations, projected on the lens plane (gray shading). The aligned sheet is located at x = 0, with a DM change shown in the top panel. Two background sources, a and b, pass the sheet at different angles (red and blue lines). Right: the observed DM change (top) and magnification (bottom) of sources a and b. The source that passes the sheet with larger ϕ shows a longer-duration ESE. A much larger DM fluctuation would be necessary to produce long-duration ESEs using a spherical lens rather than a sheet, as shown by the yellow dashed line in panel (b).