adsabs/AstroCLIMB huggingface dataset:
Paper: Dual Perspectives on GX 17+2: A Simultaneous NICER and NuSTAR Study
Authors: Malu Sudha, Renee M. Ludlam, Jeroen Homan, Dacheng Lin, Benjamin Coughenour, Edward M. Cackett
Figure caption: The variation of spectral parameters kTin, kTBB, Rin, and DISKBB normalization across the HB, HA, NB, SA, FB lower, and FB upper. Rin for the obs2 HB has been plotted without error bars to aid in proper viewing of all points. This is done because of the extremely large uncertainty on this point.
Paper: Dual Perspectives on GX 17+2: A Simultaneous NICER and NuSTAR Study
Authors: Malu Sudha, Renee M. Ludlam, Jeroen Homan, Dacheng Lin, Benjamin Coughenour, Edward M. Cackett
Figure caption: NICER + NuSTAR spectra representative of each branch with the constituent models of the best fit along with the ratio of data to best-fit model. Note that HA is obtained only from NuSTAR observations and it does not have simultaneous NICER observations.
Paper: Dual Perspectives on GX 17+2: A Simultaneous NICER and NuSTAR Study
Authors: Malu Sudha, Renee M. Ludlam, Jeroen Homan, Dacheng Lin, Benjamin Coughenour, Edward M. Cackett
Figure caption: Ratio of NuSTAR FPMA data to continuum model indicating the presence of an Fe K line emission at ∼6.7 keV. The continuum is modeled by a Diskbb+bbody+powerlaw model. Variation in the Fe K strength as it moves along the different branches can be clearly noted.
Paper: Diffusion Coefficients of WIND/STICS Protons from Diffusive Shock Acceleration with Finite Escape Boundaries
Authors: Johann R. Mejia-Ott, Brent M. Randol
Figure caption: Angle-averaged VDF and fitted curves given by the L-M method, for the shock on 2002 April 23.
Paper: Diffusion Coefficients of WIND/STICS Protons from Diffusive Shock Acceleration with Finite Escape Boundaries
Authors: Johann R. Mejia-Ott, Brent M. Randol
Figure caption: Omnidirectional VDF and solar wind parameters about a shock on 2002 April 23 05:00:00 UT, in the range ±3 · 107 km.
Paper: Diffusion Coefficients of WIND/STICS Protons from Diffusive Shock Acceleration with Finite Escape Boundaries
Authors: Johann R. Mejia-Ott, Brent M. Randol
Figure caption: Angle-averaged VDF and fitted curves given by the L-M method, for the shock on 2001 April 4.
Paper: Diffusion Coefficients of WIND/STICS Protons from Diffusive Shock Acceleration with Finite Escape Boundaries
Authors: Johann R. Mejia-Ott, Brent M. Randol
Figure caption: Omnidirectional VDF and solar wind parameters about a shock on 2001 April 4 14:39:00 UT, in the range ±7.5 · 106 km.
Paper: Probing Starspot Dynamics on the Active M Dwarf TIC 272272592: A Multiyear TESS Study
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram, Dorothy M. Mwanzia
Figure caption: The relationship between total flare energy (top) with the rotational phase of TIC 272272592. It is to be noted that no significant correlation was found between them. The bottom panel shows the occurrence of flares with the proximity of spots at different threshold values of phase difference. The threshold value of phase difference is mentioned in the figure’s title.
Paper: Probing Starspot Dynamics on the Active M Dwarf TIC 272272592: A Multiyear TESS Study
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram, Dorothy M. Mwanzia
Figure caption: This figure represents the positions, sizes, and contrast of spots in the Aitoff projection (at phase = 0 with TBJD = 2797.96 days) of TIC 272272592 in sector 55 for each modulation mentioned below the figures.
Paper: Probing Starspot Dynamics on the Active M Dwarf TIC 272272592: A Multiyear TESS Study
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram, Dorothy M. Mwanzia
Figure caption: This figure represents the positions, sizes, and contrast of spots in the Aitoff projection (at phase = 0 with TBJD = 2769.91 days) of TIC 272272592 in sector 54 for each modulation mentioned below the figures.
Paper: Probing Starspot Dynamics on the Active M Dwarf TIC 272272592: A Multiyear TESS Study
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram, Dorothy M. Mwanzia
Figure caption: This figure represents the positions, sizes, and contrast of spots in the Aitoff projection (at phase = 0 with TBJD = 1711.37 days) of TIC 272272592 in sector 15 for each modulation mentioned below the figures.
Paper: Probing Starspot Dynamics on the Active M Dwarf TIC 272272592: A Multiyear TESS Study
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram, Dorothy M. Mwanzia
Figure caption: This figure represents the positions, sizes, and contrast of spots in the Aitoff projection (at phase = 0 with TBJD = 2420.0 days) of TIC 272272592 in sector 41 for each modulation mentioned below the figures.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: In Figures 2–6, we show the bright-state (blue) and dim-state (orange) SDSS spectra for the 34 He II “changing-look” quasars identified in Section 2.3. All spectra have been smoothed using a 5 pixel boxcar kernel. The shaded gray region marks the location of the He II λ4686 broad emission line. Each panel is labeled with the object name and the observation dates of the two spectral epochs. The corresponding g-band light curve is shown below each spectrum, combining SDSS photometry (cyan), synthetic magnitudes from SDSS spectroscopy (black), Pan-STARRS (blue), and ZTF (purple) data. The observation dates of the bright- and dim-state spectra are marked by vertical blue and orange lines, respectively, in the light-curve panels.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: Two example artificial spectra (upper and lower panels) generated by adding random Gaussian noise to a real SDSS quasar spectrum with strong Fe II emission (SDSS J090112.04+011549.5). In the left panels, the host-subtracted spectra are shown in blue, with the best-fit power-law continuum and power-law plus Fe II components overplotted in green and yellow, respectively. The red lines indicate the residual spectra after subtracting the model continuum. Vertical dotted lines mark the position of the He II 4686 emission line. In the right panels, the residual spectra are replotted alongside the corresponding best-fit He II and Hβ emission-line models. This figure illustrates the degeneracy between Fe II and He II 4686, and highlights how inaccurate Fe II modeling can lead to spurious broad He II features in the residual spectrum.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: Zoom-in view of the He II-Hβ-[O III] region after subtracting the continuum, host galaxy, and Fe II emission. The shaded gray region marks the location of the He II λ4686 broad emission line. Each panel shows the spectral fitting results for a He II “changing-look” quasar in its bright state (left, blue) and dim state (right, orange). In each subpanel, the observed spectra (faint blue/orange lines) and total best-fit models (thick blue/orange lines) are shown. The best-fit Gaussian components are also shown, with the He II emission lines highlighted in red, and other features (Hβ and [O III]) indicated in black.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption:  The SDSS spectra and light curves for the 34 He ii “changing-look” quasars, see Figure 6 for details.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: The g-band variability amplitude (σrms) of our He II λ4686 “CL” quasars (orange) is shown in comparison with that of the parent sample (black; see Section 2.1). For reference, the Hβ “CL” quasars compiled from the literature are also overplotted (blue). The continuum variability of the Hβ and He II “CL” quasars is statistically indistinguishable (p = 0.672, Kolmogorov–Smirnov test), and both populations exhibit significantly stronger variability than the parent sample (p = 9 × 10−10 for He II “CL” quasars and 2 × 10−6 for Hβ “CL” quasars).
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: Histogram of the broad He II flux variation amplitude in our He II “changing-look” quasars, defined as the ratio of line flux in the dim to bright state (Flow/Fhigh). For comparison, we also show the distribution of broad Hβ flux variation amplitudes for Hβ “changing-look” quasars previously identified from SDSS spectroscopy. Vertical lines mark the median values of the two samples. The two distributions are statistically consistent, showing no significant difference in variability amplitude (Kolmogorov–Smirnov test p = 0.673).
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: The broad He II flux variability amplitude (between the bright and dim states) is plotted against that of the broad Hβ for our He II “CL” quasars, with Hβ “CL” quasars overplotted for comparison. To mitigate large statistical fluctuations caused by the typically much weaker He II line in the dim state, both variability amplitudes are derived from the median values of Monte Carlo simulations. The corresponding uncertainties represent the 68% confidence intervals.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: The bright-state Eddington ratios as a function of redshift for both He II and Hβ “changing-look” quasars are shown, with black dots indicating the parent sample defined in Section 2.1. The corresponding histograms are presented in the right panel.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: The dim-state 5100 Å host fraction as a function of redshift is shown for both He II and Hβ “changing-look” quasars. Black dots indicate the parent sample defined in Section 2.1. The host fraction is defined as the ratio of the host flux to the total flux, both measured within the 5080–5130 Å wavelength range. The corresponding histograms are shown in the right panel.
Paper: A Sample of He II λ4686 “Changing-look” Quasars
Authors: Wen-Tao Lu, Jun-Xian Wang
Figure caption: The distribution of high-state spectral S/N ratios is shown for He II “CL” quasars (yellow solid line), compared to the parent sample (gray dotted line) constructed in Section 2.1.
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: Cylindrically integrated, compensated velocity power spectra, ﹩{{ \mathcal P }}_{u}(k)﹩, as a function of wavenumbers parallel to the static gravitational potential ∇ϕ (Equation (8); k∥ = ∣kz∣; top row) and perpendicular to it (﹩{k}_{\perp }=\sqrt{{k}_{x}^{2}+{k}_{y}^{2}}﹩; bottom row). Each color represents either the total velocity u (green), the incompressible velocity component of the velocity us (blue), or the compressible component of the velocity uc (orange). All ﹩{{ \mathcal P }}_{u}(k)﹩ are compensated by the power in the total fluctuations ﹩{\left\langle {u}^{2}\right\rangle }_{{ \mathcal V }}﹩ (Equation (23)), and k−2 for Burgers-type turbulence (J. Burgers (1948). The us spectra approximately follow ∼k−3/2 scaling and uc spectra a ∼k−2 scaling, per the J. Burgers (1948) expectation for Fourier transforms of velocity discontinuities (all exponents are reported in Table 2). A shaded gray region is shown where the inertial range, ﹩\varepsilon ={\rm{const.}}﹩, is very approximately true (see Appendix C).
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: Two-dimensional slices parallel to ∇ϕ, through the center of the simulation domain, for the mass density, ρ (top row), incompressible (solenoidal) velocity, us (∇ · us = 0; middle row), and compressible velocity, uc (∣∇ × uc∣ = 0; bottom row) at three different time realizations through the evolution of the simulation. All quantities are normalized by either the volume average, in the case of the mass density ﹩{\left\langle \rho \right\rangle }_{{ \mathcal V }}﹩, or the volume-weighted rms, for the velocities. The time of each snapshot is indicated in the panel on the middle row. The first snapshot is taken close to the beginning of the simulation, t ≈ 4t0, the second just before the stationary state, t ≈ 30t0, and the final in the stationary state, t ≈ 37t0 (see the full evolution of the turbulent Mach in Figure 3, which explicitly shows a steady state is reached within t ∼ 20t0). We show the calculated gaseous scale height, ℓ0, with dashed white lines in the top left panel, as well as the midplane and 2ℓ0 with more transparent white lines. Fluctuations in ρ and uc are spatially correlated, with uc generation corresponding to the expanding shock fronts (∇ · u < 0) and the dilating regions inside of the remnants (∇ · u > 0). However, us is more closely correlated with the post-shock regions and internal SNe structures, where the SNs generate intense regions of vorticity as they expand, eventually contributing to the vortical winds coming out of the disk.
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: Evolution of the global, volume-weighted turbulent Mach number, ﹩{ \mathcal M }﹩ (Equation (14)), plotted as a function of the turbulent turnover time, t0 = 2.9 ± 0.7 Myr (Equation (15)), with each color indicating a different linear grid resolution. The turbulence reaches a steady state for t ≳ 27t0. The shaded region marks the steady state over which all of the results in this study are taken, unless explicitly stated otherwise, for which the ISM is at ﹩{ \mathcal M }\approx 1.8﹩, i.e., transonic, consistent with radio observations of the Milky Way’s ISM (B. M. Gaensler et al. 2011).
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: Two-dimensional, time-averaged pressure-density (top panel) and temperature-density (bottom panel) probability distribution functions, illustrating the presence of a multiphase ISM with a hot T ≥ 106 K (HIM) phase and volume-filling warm T ∼ 104 K (WIM) and T  ≲  104 K (WNM) phases, as annotated on each of the panels. All parameters have been normalized by their initial midplane values, ρ0 = 2.1 × 10−24 g cm−3, P0/kB = 1.6 × 10−4 K cm−3, and T0 = 12,891 K. We plot example adiabats P ∝ ργ and isotherms P ∝ ρ in both panels. Due to the lack of explicit cooling to T ≤ 104 K temperatures (see Figure 1), the T  ≲ 104 K gas is reached only through the adiabatic cooling from expanding gas in the disk, highlighted with a blue adiabat from T ∼ 104 K to T ∼ 102 K in the top panel. The distributions have been averaged over all realizations in the steady state (see Section 2.2).
Paper: So Long Kolmogorov: The Forward and Backward Turbulence Cascades in a Supernovae-driven, Multiphase Interstellar Medium
Authors: James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz, Christoph Federrath
Figure caption: The heating and cooling curve we employ in our simulation. The black solid line is the total cooling, Λ, at nH = 1 cm−3 and Z = Z⊙. Each component of the total cooling is plotted for the same density and metallicity in colored lines, labeled by the associated physical process. The gray line is the total cooling at the indicated lower density, showing that the gas density only significantly influences the cooling at T  ≲ 104 K. The black, dashed–dotted line is the total photoheating, ﹩{ \mathcal H }﹩, at gas density nH = 1 cm−3.
Paper: Rotation of Polarization Angle in Gamma-Ray Burst Prompt Phase. III. The Influence of the Magnetic Field Orientation
Authors: Xing-Yao Wang, Jia-Sheng Li, Mi-Xiang Lan
Figure caption: The variations of ΔPA with key parameters and the PA rotation spectra for various δ values. The (a), (b), and (c) panels correspond to the variations of ΔPA with q, θj, and Γ0, respectively. The (d), (e), and (f) panels correspond to the ΔPA spectra with q = 2/3,  1.2, and 1.3, respectively. In each panel, the different colored lines correspond to different δ values.
Paper: Rotation of Polarization Angle in Gamma-Ray Burst Prompt Phase. III. The Influence of the Magnetic Field Orientation
Authors: Xing-Yao Wang, Jia-Sheng Li, Mi-Xiang Lan
Figure caption: Distribution of ΔPA in the (q, θjΓ0) plane. The panels (a), (b), (c), (d), (e), (f), (g), and (h) correspond to the field orientations (δ) of 30°, 45°, 60°, 75°, 0°, 90°, 120°, and 150°, respectively. In each panel, the red dashed and blue dashed reference lines are the boundaries of the parameter space with ΔPA > 10°. In the upper-right corner of each panel, the orientation of the corresponding aligned field on the jet surface is shown.
Paper: Near-Sun Characteristics of a CME Inferred from Observations in the 5303 Å Coronal Emission Line
Authors: V. Muthu Priyal, R. Ramesh, Jagdev Singh, K. Sasikumar Raja, N. Gopalswamy
Figure caption: Panel (a): coronal image on the west limb of the Sun in the 5303 Å emission line on 2024 September 13 during the period 00:30–01:05 UT, using raster scan data with VELC. The red arc represents the solar limb (r = 1R⊙). The black area with circular edge in the image is the VELC occulter (r = 1.06R⊙). Solar north is straight up, and west is to the right. The bright and radially elongated structure seen inside the red box is the CME discussed in the main text. Its position angle (θ), measured in the counterclockwise direction from solar north, is ≈270∘. The restricted FoV in the north and south directions is due to SNR issues (J. Singh et al. 2025). Numbers 1 and 2 represent the observed enhanced emission due to the CME and activity in the adjacent region, respectively. Panel (b): contour version of the coronal image in (a). The red arrow indicates the bright structure inside the red box in (a). Panel (c): same as (a), but the image period is 01:15–01:50 UT. The structure seen inside the red box has changed and dimmed to a large extent as compared to (a). The coronal region enclosed within the red boxes and the dimensions of the boxes are the same in both cases. Panel (d): contour version of the coronal image in (c). The bright structure and its absence can be noticed more clearly in the contour images in (b) and (d).
Paper: Near-Sun Characteristics of a CME Inferred from Observations in the 5303 Å Coronal Emission Line
Authors: V. Muthu Priyal, R. Ramesh, Jagdev Singh, K. Sasikumar Raja, N. Gopalswamy
Figure caption: Left panel: 5303 Å emission spectrum related to the observations in Figure 1, at different epochs and distances. The lower most bright emission, indicated 1 in each spectrum, corresponds to the CME shown inside the red box in Figure 1. The brighter emission indicated 2 corresponds to the coronal structure indicated by the same number in Figure 1. Its intensity has decreased more rapidly (compared to the CME associated emission 1) that it is absent in the spectrum obtained around ≈01:00 UT at r = 1.43R⊙ (lower left panel). Note that different color scales are used in each of the four spectra to show the emission features with good contrast. Right panel: Spectral profiles corresponding to the bright emission indicated 1 in each spectrum shown in the left panel. The data points in the profiles are flux values in every 7th pixel of the corresponding spectra. The peak emission flux and line width at each epoch and distance are mentioned.
Paper: Near-Sun Characteristics of a CME Inferred from Observations in the 5303 Å Coronal Emission Line
Authors: V. Muthu Priyal, R. Ramesh, Jagdev Singh, K. Sasikumar Raja, N. Gopalswamy
Figure caption: Panel (a): close-up view of the SDO/AIA 131 Å difference image of the Sun near its southwest limb on 2024 September 13. The inner black arc represents the solar limb (r = 1R⊙). The outer black arc indicates the extent of the VELC occulter (r = 1.06R⊙). Panel (b): same as the image in (a) but at later epoch. The vertical red line indicates the VELC raster position at 00:35 UT. The propagating bright emission beyond the VELC occulter in the two images corresponds to the CME discussed in the main text.
Paper: Near-Sun Characteristics of a CME Inferred from Observations in the 5303 Å Coronal Emission Line
Authors: V. Muthu Priyal, R. Ramesh, Jagdev Singh, K. Sasikumar Raja, N. Gopalswamy
Figure caption: SDO/AIA 131 Å difference images showing the propagation of the CME mentioned in the main text. The inner black arc represents the solar limb (r = 1R⊙). The outer black arc indicates the extent of the VELC occulter (r = 1.06R⊙). The vertical red line in each image indicates the VELC raster position at the epoch of observations, i.e., the latter time indicated in the respective titles. The images in panels (a)–(e) and (f) are during the VELC first and second raster scan periods, respectively.
Paper: Near-Sun Characteristics of a CME Inferred from Observations in the 5303 Å Coronal Emission Line
Authors: V. Muthu Priyal, R. Ramesh, Jagdev Singh, K. Sasikumar Raja, N. Gopalswamy
Figure caption: Peak flux, width, and Doppler velocity corresponding to the 5303 Å emission line from the CME in panel (a) of Figure 1, as a function of distance in the VELC FoV. The nonthermal velocity in the line widths is shown in the right-hand-side y-axis for the middle panel.
Paper: Near-Sun Characteristics of a CME Inferred from Observations in the 5303 Å Coronal Emission Line
Authors: V. Muthu Priyal, R. Ramesh, Jagdev Singh, K. Sasikumar Raja, N. Gopalswamy
Figure caption: Scatterplot of the nonthermal velocities against the Doppler velocities for the observed 5303 Å emission line from the CME. The correlation coefficient (CC) between the two parameters is 0.9.
Paper: Mapping the SO2 Shoreline in Gas Giant Exoplanets
Authors: Ian J. M. Crossfield, Eva-Maria Ahrer, Jonathan Brande, Laura Kreidberg, Joshua Lothringer, Caroline Piaulet-Ghorayeb, Jesse Polman, Luis Welbanks, James Kirk, Diana Powell, Niloofar Khorshid
Figure caption: SO2 abundance averaged from 1 to 100 μbar for our nominal model grid (color map), with the 1 ppm volume mixing ratio indicated by the dashed line. We term this the “SO2 shoreline,” below which SO2 is unlikely to be detectable. Markers show the shoreline in the context of exoplanets observed by JWST in transit with RP ≥ 1.8R⊕. Empty symbols indicate unpublished observations, white hexagons show SO2 nondetections, and blue hexagons show SO2 detections. All four nondetections within the SO2-rich region still allow for the presence of significant levels of SO2.
Paper: Mapping the SO2 Shoreline in Gas Giant Exoplanets
Authors: Ian J. M. Crossfield, Eva-Maria Ahrer, Jonathan Brande, Laura Kreidberg, Joshua Lothringer, Caroline Piaulet-Ghorayeb, Jesse Polman, Luis Welbanks, James Kirk, Diana Powell, Niloofar Khorshid
Figure caption: Top: cross sections of sulfur-bearing species, calculated at 1000 K and 10 mbar. The data have been smoothed for clarity. Bottom left: abundance profiles for Teq = 1000 K, Tint = 100 K, 30× solar metallicity, and nominal high-energy irradiation and C/O ratio. Bottom right: full synthetic transmission spectrum (black line) together with model spectra including only one molecular absorber at a time (colored lines). Molecules not listed contribute negligibly to this spectrum.
Paper: Mapping the SO2 Shoreline in Gas Giant Exoplanets
Authors: Ian J. M. Crossfield, Eva-Maria Ahrer, Jonathan Brande, Laura Kreidberg, Joshua Lothringer, Caroline Piaulet-Ghorayeb, Jesse Polman, Luis Welbanks, James Kirk, Diana Powell, Niloofar Khorshid
Figure caption: Representative temperature profiles of our models, showing two metallicities and two Tint for equilibrium temperatures of 250, 700, 1150, 1600, and 2050 K. Changing Tint affects the temperature profile at P ≳ 1 mbar, at altitudes below where transmission spectra probe and where SO2 is produced.