adsabs/AstroCLIMB huggingface dataset:
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: The arrival time delay, τ, in observed days (Fermat potential) relative to image 1 of the LCE knot. Images of the same source position form at stationary points in the Fermat potential (minima, maxima, and saddle points). The southeast arc image forms first (image 12), followed by the north arc (images 1–6), the northwest arc (images 7–10), and the west arc (image 11).
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: The cumulative projected mass density profile at the core of the lensing cluster PSZ1 G311.65−18.48. The functional 1σ uncertainty (statistical) is shown in the bottom panel.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Same as Figure 5, zoomed in on the north arc (images 1–6 of the source). North is up, east is left.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Zoomed-in view of the giant arcs of the Sunburst system. The color frames are a composite of F140W (R), F606W (G), and F410M (B), probing the rest-frame optical, UV continuum, and Lyα, respectively. The filters, scaling, brightness, and saturation levels were chosen to emphasize color variations between emission knots. In each monochrome frame we label the identified emission knots. A 2.″0 scale bar is shown in the bottom frame. The gray boxes in Figure 1 indicate the location of the frames shown here within the cluster field of view.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Imaging data of PSZ1 G311.65−18.48, composed of F140W+F160W (R), F606W (G), and F390W (B). The secure and candidate multiple-image systems are labeled and color coded; candidate images are annotated with a question mark. The individual clumps within each image are not labeled, to reduce clutter. The critical curve for a source at z = 2.3703 is overlaid in red. Gray rectangles mark the giant arcs of the Sunburst Arc; they are shown in more detail in Figure 2. See also Figure 3 for zoomed-in view of the multiple images.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Close-up view of the multiple images of strongly lensed galaxies identified in the field of PSZ1 G311.65−18.48. The color image is composed of F140W+F160W (R), F606W (G), and F390W (B), chosen to highlight color gradients within the lensed galaxies to show their internal structure and color differences between galaxies. North is up, and each image is 4.″0 × 4.″0.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Demonstration of the tomographic power of the PSZ1 G311.65−18.48 lens, and an upper limit on clump sizes from the HST/ACS PSF. We show the source plane ray-traced HST/ACS F814W PSF at the image plane location of each of the images of the 19 clumps we identify in the Sunburst Arc. The colors are the same as in Figure 2. The background grid lines are separated by 0.2 kpc. The blue circle has a radius of 0.05 kpc. The unlensed HST PSF, 0.″08 = 0.69 kpc, is shown on the left for comparison.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: An upper limit on the source plane size of the LCE clump, from the HST/ACS PSF and the lensing magnification. The HST/ACS F814W PSF is ray-traced from the image plane location of each of the images of the LCE to the source plane. The background grid lines are separated by 0.02 kpc. The gray lines show the projections from 100 models that sample the parameter space, indicating statistical uncertainty; the projections of the high-uncertainty image 1.5 are not shown for clarity. The multidirectional magnification constrains the physical size of the LCE to r eff ≲ 31.6 pc, represented with a red ellipse at the center.
Paper: Solar Flare Forecast Using 3D Convolutional Neural Networks
Authors: Pengchao Sun, Wei Dai, Weiqi Ding, Song Feng, Yanmei Cui, Bo Liang, Zeyin Dong, Yunfei Yang
Figure caption: The magnetograms of AR 11158 where an X2.2-class flare erupted and the corresponding heat maps (colored images). The heat maps illustrate the contribution to the flaring-forecast category.
Paper: Solar Flare Forecast Using 3D Convolutional Neural Networks
Authors: Pengchao Sun, Wei Dai, Weiqi Ding, Song Feng, Yanmei Cui, Bo Liang, Zeyin Dong, Yunfei Yang
Figure caption: (a) The HMI image that is temporally closest to the flare peak time. (b) The AIA 193 Å image of the flare-eruption position. (c) The superposition image of panels (a) and (b).
Paper: Solar Flare Forecast Using 3D Convolutional Neural Networks
Authors: Pengchao Sun, Wei Dai, Weiqi Ding, Song Feng, Yanmei Cui, Bo Liang, Zeyin Dong, Yunfei Yang
Figure caption: The 120-frame magnetograms of each 24 hr time period were composed into eight magnetogram sequences.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Motion of Castor C relative to the barycenter of Castor AB in the R.A. and decl. directions, from visual measures made over the past two centuries. The original measures of Castor AC and BC have been reduced to the barycenter of AB. Linear fits indicated by the green lines give the slopes ﹩\delta {\mu }_{\alpha }^{* }﹩ and δ μ  δ  shown in each panel, which are a direct measure of the difference in the proper motions of Castor C and Castor AB. A few outliers have been removed for clarity.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Measured H-band and K-band primary-to-secondary flux ratios for Castor A and B with their uncertainties shown as shaded regions. The solid lines represent the predicted run of the flux ratios as a function of the age in each system at the measured masses of the components, according to the PARSEC models of Chen et al. (2014). Within the uncertainties there is good agreement between the measurements and the expected flux ratios at the age of 290 Myr (dotted line) that best fits the radius of Castor Aa in Figure 7.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Change in the position of Castor C relative to the barycenter of Castor AB from visual measures made over the past two centuries. The orbital motion of Castor A and B with respect to their barycenter has been subtracted from the original measures of Castor AC and BC, respectively. A few obvious outliers have been removed for clarity.
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Spectra for DA 530 plotted in the optical depth variable (e −τ  − 1) as a function of velocity (black) and H I emission (blue). The optical depth spectra were produced by combining the Stokes Q and U spectra, which were determined using Equation (15). 1. Top: DRAO-ST spectra, with (e −τ  − 1) spectra from the S21-2020 data and H I emission spectra from the S21-2012 data. 2. Bottom: NRAO-VLA spectra from the VLA-2004 data. The spectra are shown for four regions on DA 530: (a) the whole SNR, (b) the southwest shell, (c) the southeast shell and center, and (d) the northern shell. Shading indicates one [red], two [blue], and three [yellow] standard deviations from the unabsorbed emission line (e  τ  − 1 = 0).
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Continuum images of DA 530 observed by the NRAO-VLA. These continuum images of DA 530 show (clockwise from top left) Stokes I, polarized intensity (PI), U, and Q and were created by averaging across the end channels of the VLA-2004 data cubes. The Stokes I image includes H I emission in addition to the continuum emission from DA 530, as all frequency channels included in the observations contained some emitting H I.
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: DRAO-ST continuum images of DA 530. Images of (clockwise from top left) Stokes I, polarized intensity (PI), U, and Q made by combining the four continuum frequency channels of the C21-2020 images.
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Foreground H I column density for DA 530. The H I column density profile (red curve) was calculated using the DRAO-ST absorption profile over the whole remnant (top right plot of Figure 4). The H I emission profile (black curve) was obtained from the S21-2012 Stokes I data cube averaged in each velocity channel over the area covering the whole remnant.
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Illustration of the H I absorption method for determining the distance to an SNR. Top: The absorption by the farthest H I cloud along the line of sight indicates the minimum distance to the SNR. Bottom: The emission “off ” the SNR is subtracted from that “on” the SNR in order to remove excess H I emission and self-absorption structures from the spectrum.
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Velocity profile for the LOS toward DA 530 determined with the kinematic distance tool by Foster & MacWilliams (2006). This tool enables improved kinematic distance estimates by taking the different velocity features along the LOS into account. The kinematic distances corresponding to our absorption features at −28 km s−1 and −67 km s−1 are marked in red and blue, respectively.
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Comparison of simulated radial profiles based on different compression ratios with the observed radial profile of DA 530 in total intensity (Stokes I profile, left) and polarized intensity (PI profile, right). For the simulations, we used a compression ratio of 4 for the Sedov phase, 2.5 for the early free-expansion phase, and 10 for the radiative phase. Radial profiles were normalized and adjusted to the peak emission on top of the shell, as it marks the inner edge of the shell, where the LOS through the synchrotron emitting plasma is the longest. The profiles were determined over the bright emission of the northern shell from 300° to 40° (in Galactic coordinates). Here 0° and 360° is north, and the angle increases clockwise.
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Longitude–velocity image from the S21-2012 Stokes I data cube showing the H I emission in the direction of DA 530. This LOS passes through the center of the SNR at a Galactic latitude of 6.°9. There is continuous H I emission up to a velocity of about −30 km s−1 corresponding to the LOS passing through local H I gas. The LOS just brushes the top of the Outer arm at v = −75 km s−1, and at a velocity of about −110 km s−1 we see increased H I emission as the warped Galactic plane intersects the LOS (Foster & MacWilliams 2006).
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Stokes U optical depth spectra for DA 530, calculated as described in Equation (15). 1. Top: DRAO-ST Stokes U spectra from the S21-2020 U data cube. 2. Bottom: NRAO-VLA Stokes U spectra from the VLA-2004 U data cube. Shading indicates one [red], two [blue], and three [yellow] standard deviations from the unabsorbed emission line (e  τ  − 1 = 0).
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Stokes Q optical depth spectra for DA 530, calculated as described in Equation (15). 1. Top: DRAO-ST Stokes Q spectra from the S21-2020 Q data cube. 2. Bottom: NRAO-VLA Stokes Q spectra from the VLA-2004 Q data cube. Shading indicates one [red], two [blue], and three [yellow] standard deviations from the unabsorbed emission line (e  τ  − 1 = 0).
Paper: A New Distance to the Supernova Remnant DA 530 Based on H I Absorption of Polarized Emission
Authors: Rebecca A. Booth, Roland Kothes, Tom Landecker, Jo-Anne Brown, Andrew Gray, Tyler Foster, Eric Greisen
Figure caption: Magnitude of elevation, ∣z∣, above the Galactic plane for all 112 SNRs in Green’s Catalog (Green 2019) with recorded distance measurements.
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: Evolution of the rotation period of the J2211+1136 for an accretion rate of ﹩\dot{M}=2.62\times {10}^{-7}{M}_{\odot }﹩ yr−1 and for different values of initial rotational periods, P 0 = (3.14, 21.5, 41.5, 81.5, 101.5, 119.8) s. The dotted lines divide the evolution into three stages according to the value of ω. In the first stage, the WD can start with ω > 1 or ω < 1 depending whether the initial period is below or above the equilibrium period, P eq = 61.15 s (Equation (20)), respectively. For both values, the involved torques are magnetic torque, T mag, and accretion torque, T acc. However, T acc is the dominant torque in this phase. For ω ≈ 1, T mag ≈ T acc and the system goes through the P eq. For ω < 1, the involved torque is T mag. T acc no longer acts on the star, as in the third stage the disk has already been exhausted. The upper dashed line indicates the current rotation period of the WD.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption: Comparison of arc-based curvature estimate (η p ) with ISS-parameter-based curvature (η iss ) for secondary spectra using normalized (p, q) coordinates. All three panels are plotted to the same limits in p and q and hence can be directly compared. The dashed line follows the η p parabola; the solid line indicates the η iss parabola. (a) B0450–18 observed at 825 MHz (Figure Set 1.3). (b) B1508+55 observed at 340 MHz (Figure Set 1.11). (c) B2310+42 observed at 340 MHz (Figure 2 and Figure Set 1.21).
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: ∣T acc∣ and ∣T mag∣ as a function of ω > 1 where we considered a WD with B = 100 MG, ﹩\dot{M}={10}^{-7}\,{M}_{\odot }﹩ yr−1, and a quadrupole-to-dipole magnetic field strength ratio B quad/B. The ratio B quad/B = 0.0 corresponds to the case of a pure dipole magnetic field.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption: Dual frequency comparison of secondary spectra using normalized (p, q) coordinates. (a) B2021+51 at 340 MHz. Display is a linear gray scale for the DS and logarithmic gray scale for the SS, covering about 50 dB from white to black. A pq arc (p = q 2) is superposed on the SS. Since p and q are normalized by the angular width of the corresponding B(θ) curves, the axis stretch factors are accounted for automatically. (b) B2021+51 at 825 MHz observed 5 days later than that in the left panel. Display style is the same as in panel (a). (c) Same data as in (b), but with Gaussian white noise added to approximately match the S/N ratio of panel (a).
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: ∣T acc∣ and ∣T mag∣ as a function of ω < 1 where we considered a WD with B = 100 MG, ﹩\dot{M}={10}^{-7}\,{M}_{\odot }﹩ yr−1, and a quadrupole-to-dipole magnetic field strength ratio B quad/B = 0.0, since the effect of the quadrupole magnetic field is very small when we take into account the values of ω < 1 presented here (See Equation (15)).
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption: Theoretical secondary spectra for strong scattering in a screen with an isotropic Kolmogorov phase spectrum. Left: normalized variables set at 825 MHz. Right: stretched to 340 MHz; times 825/340 = 2.4 in Doppler; and times (825/340)4 = 35 in delay. They are displayed over equal ranges in Doppler and 4 times larger in delay; dynamic range in gray scale is set to 60 dB in both.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption: Histogram of arc power asymmetry index defined as κ ≡ (R − L)/(R + L), where R is the arc power for f  D  > 0, and L is the arc power for f  D  < 0. Negative values of κ represent scattering material out in front of the projected path of the pulsar across the sky.
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: Accretion rate as a function of cooling age, calculated from Equation (24), for J2211+1136. The WD parameters are M = 1.27 M ⊙, R = 3.21 × 108 cm, and P obs = 70.3 s. The dipole magnetic field is B = 15 MG and θ = 90°.