adsabs/AstroCLIMB huggingface dataset:
Paper: The Formation and Evolution of Dust in the Colliding-wind Binary Apep Revealed by JWST
Authors: Yinuo Han, Ryan M. T. White, Joseph R. Callingham, Ryan M. Lau, Benjamin J. S. Pope, Noel D. Richardson, Peter G. Tuthill
Figure caption: Linear fits to the shell radius as a function of shell order used to determine the intershell spacing along different position angles from the binary.
Paper: The Formation and Evolution of Dust in the Colliding-wind Binary Apep Revealed by JWST
Authors: Yinuo Han, Ryan M. T. White, Joseph R. Callingham, Ryan M. Lau, Benjamin J. S. Pope, Noel D. Richardson, Peter G. Tuthill
Figure caption: Spitzer observations of Apep at 7.9 μm. The direction orthogonal to the line of nodes (R. M. T. White et al. 2025) is indicated with dashed lines and uncertainty range with dotted lines.
Paper: The Serpent Eating Its Own Tail: Dust Destruction in the Apep Colliding Wind Nebula
Authors: Ryan M. T. White, Benjamin J. S. Pope, Peter G. Tuthill, Yinuo Han, Shashank Dholakia, Ryan M. Lau, Joseph R. Callingham, Noel D. Richardson
Figure caption: The free parameters of Equations (B14) and (B15) change the depth and breadth of the strength variations in dust production. The top axis represents the weighting applied to each ring as a function of true anomaly for a representative set of free parameters, while the bottom axis represents the weighting applied to each particle within each single ring.
Paper: The Formation and Evolution of Dust in the Colliding-wind Binary Apep Revealed by JWST
Authors: Yinuo Han, Ryan M. T. White, Joseph R. Callingham, Ryan M. Lau, Benjamin J. S. Pope, Noel D. Richardson, Peter G. Tuthill
Figure caption: Linear fits to the inner shell radius as a function of time used to determine the expansion speed in different directions from the binary.
Paper: microJAX: A Differentiable Framework for Microlensing Modeling with GPU-accelerated Image-centered Ray Shooting
Authors: Shota Miyazaki, Hajime Kawahara
Figure caption: An example of a triple-lens configuration with parameters (q, s, q3, r3, ψ, ρ) = (0.5, 1.1, 0.91, 1.46, 0.1) and source center wcenter = (0, 0.1). The red and green curves represent the caustics and critical curves, respectively, and the black points indicate the lens positions. The source limb is sampled with Nlimb = 500 points (blue), which are mapped to the image plane, producing six distinct images (purple). For each image, a polar-coordinate region is defined based on the image-limb points, within which a uniform 50 × 50 grid is placed for integration. Grid points falling inside the source are marked in orange, while those outside are shown in gray.
Paper: microJAX: A Differentiable Framework for Microlensing Modeling with GPU-accelerated Image-centered Ray Shooting
Authors: Shota Miyazaki, Hajime Kawahara
Figure caption: Relative accuracy of microJAX magnification estimates compared to VBBinaryLensing, as a function of source size (ρ = 0.1 to 10−4) and angular resolution (Nθ = 500, 1000, 8000) with fixed Nr = 1000. Each panel shows the relative error in magnification computed by microJAX, to the reference values from VBBinaryLensing, for 1000 randomly sampled source positions near the central caustic of a binary lens with q = 0.1 and s = 1. A uniform-brightness source is assumed, and VBBinaryLensing is run at a relative accuracy of 10−5. The bottom right panel illustrates the spatial distribution of test points near the caustic.
Paper: microJAX: A Differentiable Framework for Microlensing Modeling with GPU-accelerated Image-centered Ray Shooting
Authors: Shota Miyazaki, Hajime Kawahara
Figure caption: The top panel shows the triple-lens magnification curve for a uniform-brightness source, with the inset displaying the corresponding caustic structure (red solid line) and source trajectory (blue solid line), where the microlensing parameters are (t0, tE,u0, q, s, α, q3, r3,ψ) = (0, 10 days, 0, 0.5, ﹩1.1,60^\circ ,0.03,1.24,76\mathop{.}\limits^{^\circ }0)﹩. The subsequent panels show the gradients of the magnification for each microlensing parameter. The resolutions of the inverse ray grid are (Nr, Nθ) = (500, 500), respectively.
Paper: microJAX: A Differentiable Framework for Microlensing Modeling with GPU-accelerated Image-centered Ray Shooting
Authors: Shota Miyazaki, Hajime Kawahara
Figure caption: Geometrical configuration of the triple-lens system used in magnification and gradient calculations. The primary and secondary lenses (M1, M2) are separated by s ≡ 2a along the horizontal axis, with the origin ﹩{ \mathcal O }﹩ defined as their barycenter. The source (blue line) moves with impact parameter u0 and angle α relative to the binary axis. The third lens M3 is placed at polar coordinates (r3, ψ) relative to the midpoint between M1 and M2.
Paper: Converging on the Cepheid Metallicity Dependence: Implications of Nonstandard Gaia Parallax Recalibration on Distance Measures
Authors: Louise Breuval, Gagandeep S. Anand, Richard I. Anderson, Rachael Beaton, Anupam Bhardwaj, Stefano Casertano, Gisella Clementini, Mauricio Cruz Reyes, Giulia De Somma, Martin A. T. Groenewegen, Caroline D. Huang, Pierre Kervella, Saniya Khan, Lucas M. Macri, Marcella Marconi, Javier H. Minniti, Adam G. Riess, Vincenzo Ripepi, Martino Romaniello, Daniel Scolnic, Erasmo Trentin, Piotr Wielgórski, Wenlong Yuan
Figure caption: P–L intercept β, where ﹩M=\alpha \,(\mathrm{log}P-1)+\beta ﹩, in the [3.6 μm] filter for Milky Way cluster Cepheids (red), the sample of 10 bright Cepheids with HST FGS parallaxes from B07 (yellow), LMC Cepheids (blue), and Cepheids in different regions of the SMC (green). The red “X” shows the P–L intercept obtained after the MF25 recalibration of Gaia EDR3 parallaxes. The metallicity on the horizontal axis is expressed in [O/H] for a direct comparison with abundances in SNIa host galaxies (gray histogram). The slope of the gray line represents a γ ∼ −0.23 mag dex−1 metallicity dependence obtained by fitting a straight line through the MW, LMC, and SMC. Conversely, the γ ∼ 0 result by MF25 is obtained from a comparison between the MW red “X” marker, the LMC, and the SMC dark green “X” marker, which align with a horizontal line.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 4 but for the radiation-dominated regime with different U/(n1T2) (panels (a)–(c)). A fraction of grains are rapidly driven to the high-J attractor, and some grains are driven to the low-J rotation and trapped (confined) there by strong RATs. The confinement area is smaller for higher U/(n1T2). Collisional and magnetic excitations strongly disturb grain alignment but cannot scatter them into high-J rotation. Rotational disruption can occur for weak grains of ﹩{S}_{{\rm{\max }},{\rm{7}}}=0.01﹩ (pink dotted line), even when grains are not yet reaching a high-J attractor.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: The fraction of grains with initial random orientation that undergo fast alignment with high-J, ﹩{f}_{{\rm{high}}-{\rm{J}}}^{{\rm{fast}}}﹩, for different RAT parameters and magnetic relaxation, assuming ψ = 0° for the different radiation fields U/(n1T2) (panels (a)–(d)). The value of ﹩{f}_{{\rm{high}}-{\rm{J}}}^{{\rm{fast}}}﹩ increases with δmag except for U/(n1T2) = 15,640 where magnetic relaxation becomes ineffective, and alignment is dominated by RATs.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: The phase trajectory map for the RAT model ﹩{q}^{{\rm{\max }}}=2﹩ and SPM grains with δmag = 103 in extreme radiation fields with different U/(n1T2) (panels (a)–(d)). The fraction of grains with fast alignment at high-J attractor decreases with increasing U/(n1T2) due to reduced efficiency of magnetic relaxation. The trajectory of grains during low-J rotation is disturbed less, and the confinement area is narrower, for higher U/(n1T2) due to stronger RATT. Rotational disruption can occur even when grains are still on the way to the high-J attractor.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 6 but for the time-dependent alignment degrees. Within a time t ∼ 0.01τdamp, the external and net alignment degrees (QJ, R) increase rapidly due to external alignment by MRATs, but the internal alignment degree QX decreases due to the damping of the grain angular momentum. Afterward, the alignment degrees decrease and slowly change after t ∼ 0.02τdamp ∼ 0.02τgas due to radiative torque trapping, although the external alignment is still fluctuating due to gas and magnetic excitation.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 4 but for PM grains with δmag = 1 and the RAT model without high-J attractor of ﹩{q}^{{\rm{\max }}}=1﹩. The phase trajectory during the low-J rotation is significantly disturbed by collisional and magnetic excitations. All grains have cyclic trajectories during the suprathermal state of J/I1ωT > 3 and randomly during J/I1ωT < 3 due to gas and magnetic excitations.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 4 but for PM grains with δmag = 1. The phase trajectory during the low-J rotation is strongly disturbed by collisional and magnetic excitations, but the trajectory for suprathermal rotation of J/I1ωT > 3 is deterministic due to reduced magnetic relaxation. All grains eventually reach the high-J attractor (red circle) by MRATs due to gas and magnetic excitations.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 5 but for PM grains with δmag = 1 and ﹩{q}^{{\rm{\max }}}=1﹩. The net alignment degree R is zero due to collisional randomization for the RAT model without high-J attractors, but the internal alignment degree is still finite with QX ∼ 0.2.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 12 but for time-dependent alignment degrees. Grain alignment degrees decrease with increasing U/(n1T2) due to reduced efficiency of magnetic relaxation. Fluctuations of external alignment QJ (blue line) caused by gas and magnetic excitations at low-J rotation is much weaker for stronger radiation fields due to RATT effect.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 5 but for PM grains with δmag = 1. The alignment degrees increase with time, but the time required to reach nearly perfect alignment is longer with TPA ∼ 40–70τdamp due to the reduced magnetic excitations.
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Data sample used in this study. Panel (a): CMD of the data sample in Section 2.1 using AvdM10 photometry. The blue region defines the selection of warm HB stars. The black dotted line shows the ZAHB track from the BaSTI model (see Section 2.3.1 for details). Panel (b): VLOS distribution of the warm HB stars and all other stars. The gray histogram indicates stars excluded based on the selection criteria for the two samples. Panel (c): proper motion distribution of the same samples, with colors corresponding to panel (b). Panel (d): reestimated S/N distribution in the Na I D region. Panels (e) and (f): example MUSE spectra (black line) of warm HB and all other stars, with the S/N and VLOS indicated in the top left corner. The green lines show the residuals between the observed spectra and the best-fit SPEXXY model from N23. Vertical lines are the positions of the Na I D absorptions from foreground (solid, located at 0 kms−1) and intracluster (dashed, at 232.7 kms−1) atomic gas of ω Cen. An additional contribution from the stellar photosphere, seen as the right-most absorption feature, is present in panel (f).
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Spatial distribution of EWD2,ISM from the foreground Na atomic gas. The left panel shows individual measurements from the original spectra of warm HB stars. The right panel shows measurements from Voronoi-binned SPEXXY residual spectra (N23) of all other stars. The number of stars used for each panel is noted in the subtitles. The x- and y-axes indicate coordinates in (α, δ) relative to the center of ω Cen. The two blank regions near the center of ω Cen are due to the lack of non-AO observations. Both warm HB and all other stars demonstrate clear spatial substructures of foreground Na atomic gas, and they are consistent with the differential reddening distribution from previous studies (see Section 6.2 for detailed discussion). The individual warm HB EWD2,ISM measurements and the Voronoi-binned EWD2,ISM map with uncertainties are available as a machine-readable table (columns listed in Table 1) and a FITS image, respectively.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Demonstration of spectral fitting to measure the EWs of Na I D, as described in Section 3.1. The top panel shows an example spectrum of a warm HB star, while the bottom panel shows a Voronoi-binned residual spectrum from all other stars. The equivalent widths (EWs) of the Na I D lines, in units of Å, are labeled in each panel. The red-shaded region indicates the wavelength range used for fitting. The gray-shaded regions are used to estimate the continuum (fc) in Equation (4). Fitting residuals are shown in green as a separate subpanel. The warm HB spectrum is expected to have minimal photospheric contribution to Na I D and thus we name them as “ISM” and “ICM.” For all other stars that are mostly cooler, contamination from the stellar photosphere could remain in the SPEXXY residuals. Therefore, we label the absorptions at ω Cen systemic velocity as “others.” Note that the D2 line is at a shorter wavelength than the D1 line for both the ISM and ICM/others components.
Paper: Far-ultraviolet Emission Line Investigation of Flares on AU Mic
Authors: Adalyn Gibson, Adam F. Kowalski, Adina D. Feinstein
Figure caption: The observed C II spectral lines during Flare B at different times throughout the flare (B. Rathore et al. 2015; H. Uitenbroek 2001). Models from the RH code are shown in orange (without Γ) and blue (Γ × 30). The model time step 6.0 s appears nearly flat here. However, the spectral line shape is still present, but the flux at 6.0 s is only ∼5.3% of the flux at 4.6 s. The model surface flux has been scaled to the observations and convolved to the spectral resolution of the COS/HST observations. The models are scaled by optimizing the projected solid angle of AU Mic on the sky to the observations, and each model is scaled by the same factor across time.
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: Comparison of EWD2,ISM measurements between warm HB stars and all other stars as shown in Figure 4. The gray dots represent individual warm HB stars. The y-axis represents EWD2,ISM measured from individual warm HB spectra, and the x-axis corresponds to EWD2,ISM values interpolated from the Voronoi-binned maps of all other stars, using the coordinates of the warm HB stars. The red line indicates a one-to-one relation for reference. The black line and gray-shaded region represent the median and the (16th, 84th) percentiles of the comparison, respectively. This figure indicates that although warm HB stars and all other stars show a similar structure in their spatial distributions, their one-to-one comparison reveals a systematic offset.
Paper: oMEGACat. VII. Tracing Interstellar and Intracluster Medium of ω Centauri Using Sodium Absorptions
Authors: Z. Wang, 梓先 王, A. C. Seth, M. Latour, J. Strader, M. Häberle, N. Neumayer, C. Clontz, S. Kamann, M. S. Nitschai, M. Alfaro-Cuello, A. Bellini, A. Feldmeier-Krause, M. Libralato, A. P. Milone, P. J. Smith, S. O. Souza, G. van de Ven
Figure caption: An illustration of the method used in this paper to probe the foreground interstellar medium (ISM) and intracluster medium (ICM) using the Na I D region of our MUSE spectra. The top portion shows the locations of the observer, the intervening interstellar medium, and the intracluster medium; each is labeled with its radial velocity. These differing radial velocities result in a Doppler offset between the interstellar and intracluster Na I D lines as shown in the bottom panel, which shows where we expect to see the lines from each component in our spectra.
Paper: Far-ultraviolet Emission Line Investigation of Flares on AU Mic
Authors: Adalyn Gibson, Adam F. Kowalski, Adina D. Feinstein
Figure caption: An example of a model fit to Flare R with the Llamaradas Estelares (T. Mendoza et al. 2022) analytical flare model. Flare R is the highest-energy flare in Visit 3 with E﹩{}_{{\rm{flare}}}=(1.292\pm 0.176)\times 1{0}^{31}﹩ erg. The extended enhanced tail of Flare R is not accurately captured by the model fit; the model fit underestimates the flux during the decay phase of this flare.
Paper: Far-ultraviolet Emission Line Investigation of Flares on AU Mic
Authors: Adalyn Gibson, Adam F. Kowalski, Adina D. Feinstein
Figure caption: Same as Figure 3 but for the C III emission line. We see the same behavior in C III as we do for C II. In particular, note the strong blue asymmetry in the spectrum, whereas the red wing predominantly responds in the second flare peak.
Paper: Buildup, Explosion, and Untwisting of a Solar Active Region Jet Observed with Solar Orbiter, IRIS, and SDO
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore, Sanjiv K. Tiwari, David Berghmans, Andrei Zhukov, Marilena Mierla, Cis Verbeeck, Koen Stegen
Figure caption: Schematic depictions of the minifilament flux rope eruption that makes the jet’s base brightening and the jet’s spire based on our observations and PFSS extrapolations. The drawings are schematics of the erupting and reconnecting magnetic field viewed horizontally from the south along the direction of the neutral line between the positive flux in the jet’s base and the negative flux clump that is canceling with that positive flux. The left-side negative flux in the schematic represents negative flux near the sunspot’s northwest edge in the HMI magnetograms. Panel (a) shows the onset of fast internal reconnection. Panel (b) is during the onset of fast external reconnection. The thick horizontal black line is the solar surface. Positive and negative magnetic flux polarities are labeled with plus and minus signs, respectively. Stars indicate the locations of ongoing magnetic reconnection. The curves are projections of magnetic field lines on a vertical east–west plane through the middle of the jet’s base. Red curves are projections of field lines that have undergone reconnection. Black curves are projections of field lines that have not yet undergone reconnection or that will not undergo reconnection. The sky blue cloud carried in the flux rope’s spiral field is the dark filament viewed end-on. The drawings are for the spiral field a having left-handed twist. The magenta vertical tick marks the magnetic neutral line, and the black vertical ticks mark the outer boundaries of the “plus” and “minus” fluxes. In panel (b), the solid red arrows represent plasma outflow from the reconnection out along the reconnected far-reaching field that fills the jet spire.
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: The TESS light curve and corresponding Fourier amplitude spectrum of DG Leo. Top panel: the full light curve from Sector 21. Second panel: the Fourier amplitude spectrum derived from the full light curve. The dominant frequency peak at 0.4822 day−1 (red dashed vertical line) corresponds to ellipsoidal variations, while other significant peaks represent pulsation frequencies. Third panel: the light curve after removing the dominant ellipsoidal variations. Bottom panel: a zoomed-in view of the detrended light curve between TJD 1872–1876.5. (TJD = BJD − 2457000.0).
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: This visualization presents the fitting results ﹩{S}_{m}^{2}﹩ alongside key physical parameters: metallicity (Z), effective temperature (Teff), acoustic radius (τ0), stellar rotation velocity (Vrot), convective-core-to-stellar-radius ratio (Rcz/R), and overshooting parameter (fov). A red horizontal line marks the threshold ﹩{S}_{m}^{2}=0.10﹩. Black dots denote the minimum ﹩{S}_{m}^{2}﹩ for each model, while a red dot identifies the minimum ﹩{S}_{m}^{2}﹩ for the best-fitting model (Model A3).
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: The light curve of DG Leo after subtracting the binary model, along with its corresponding Fourier spectra. Top panel: the residual light curve (blue dots) with the Fourier fit model overplotted (red curve). The inset shows a zoomed-in view of the same light curve between TJD 1872 and 1874. Middle panel: the Fourier amplitude spectrum of the residual light curve; the seven independent frequencies are marked by colored vertical dashed lines. Bottom panel: the residual spectrum after prewhitening with 40 significant frequencies.
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: This visualization presents the fitting metric ﹩{S}_{m}^{2}﹩ and physical parameters: stellar mass (M), radius (R), luminosity (L), age (Age), gravitational acceleration (﹩{\mathrm{log}}g﹩), and central hydrogen abundance (Xc), with a red horizontal line marking the threshold ﹩{S}_{m}^{2}=0.10﹩, where black dots indicate the minimum ﹩{S}_{m}^{2}﹩ for each model while the red dot identifies the minimum ﹩{S}_{m}^{2}﹩ of the best-fitting model (Model A3).