adsabs/AstroCLIMB huggingface dataset:
Paper: Continuous Gravitational Waves from Magnetized White Dwarfs: Quantifying the Detection Plausibility by LISA
Authors: Mayusree Das, Banibrata Mukhopadhyay, Tomasz Bulik
Figure caption: Top panel: the decay of maximum magnetic ﹩{B}_{{\rm{\max }}}=4\times 1{0}^{13}﹩ G with time for WD1 and WD2 with radius 5708 and 2815 km, respectively. Middle: magnetic field as a function of radius, before and after magnetic field decay for toroidal field (WD1). Bottom panel: same as the middle panel, except for poloidal field (WD2).
Paper: Continuous Gravitational Waves from Magnetized White Dwarfs: Quantifying the Detection Plausibility by LISA
Authors: Mayusree Das, Banibrata Mukhopadhyay, Tomasz Bulik
Figure caption: Same as the top panel of Figure 4, except with an initial χ = 30°.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Top panel: detections (circles) and upper/lower limits (triangles) of H2 versus H I column density for the observational sample (see Section 4). Red symbols show observational constraints on the binned median H2 column densities. Middle panel: median (solid lines) and 99th percentile (dashed lines) of ﹩{N}_{{{\rm{H}}}_{2},{\rm{p}}}﹩ versus NH I,p for each redshift in our model. We show again the observed medians for the high-z sample and also Milky Way ISM sightlines from B. D. Savage et al. (1977). Bottom panel: as for the middle panel, including the analytic models described in Section 4.2 and a line denoting Rmol = 0.1 in red. Our analytic CGM model for the median curve assumes optically thin conditions and n/ILW ∝ NH I (see Equation (9)). The 99th percentile model assumes a 1D slab with n = 100 cm−3, ﹩Z{{\prime} }_{d}=0.1﹩, and ILW = 10. Our results reproduce the low H2 columns in DLAs with lower H I columns and are described well by our analytic ISM and CGM models.
Paper: Disentangling Thermal and Abundance Characteristics in a Solar Flare Using SDO/AIA, Hinode/XRT, and MinXSS-1 Observations
Authors: Xiaoyan Xie, Anna Chen, Crisel Suarez, Katharine K. Reeves, Soumya Roy, Christopher S. Moore, Nishu Karna, Joy Velasquez
Figure caption: The position-versus-time stack plots of 131 Å, 304 Å, and 171 Å distribution along the paths of C1 (top row) and C2 (bottom row) indicated in Figure 2. The distance increment corresponds to the arrow direction indicated on the paths C1 and C2. The dotted lines ca, cb, cc, and cd correspond to the crosses indicated in Figure 2. S1 indicates the ejected outflows from the brightening intersection of eruptive filament F1 and preexisting filament F2. The fitted speed of the outflows, indicated by solid lines, is 44 km s−1. The minimum and maximum fitted speeds, shown by dashed lines (K. K. Reeves et al. 2015), are 38 km s−1 and 45 km s−1, respectively.
Paper: Disentangling Thermal and Abundance Characteristics in a Solar Flare Using SDO/AIA, Hinode/XRT, and MinXSS-1 Observations
Authors: Xiaoyan Xie, Anna Chen, Crisel Suarez, Katharine K. Reeves, Soumya Roy, Christopher S. Moore, Nishu Karna, Joy Velasquez
Figure caption: SDO/AIA and Hinode/XRT response functions with coronal abundances (solid curves) and photospheric abundances (dotted lines, scaled by a factor of 3.98) for the date of 2016 July 21. Following the practice in P. J. Wright et al. (2017), XRT response functions are further multiplied by a factor of 2.
Paper: Disentangling Thermal and Abundance Characteristics in a Solar Flare Using SDO/AIA, Hinode/XRT, and MinXSS-1 Observations
Authors: Xiaoyan Xie, Anna Chen, Crisel Suarez, Katharine K. Reeves, Soumya Roy, Christopher S. Moore, Nishu Karna, Joy Velasquez
Figure caption: Left: GOES flux around the flare. Right: the evolution of Si during the flare (adapted from C. Suarez & C. S. Moore 2023), where the purple bar indicates the photospheric value with the FIP bias as 1. The dashed lines indicate the times with XRT observations, and the corresponding abundance models are labeled by different colors.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Visualization of the model convergence over 14 iterations for ILW = 1, n = 100 cm−3, ﹩{Z}_{d}^{{\prime} }=1﹩, and Ntot = 5 × 1019 cm−2. Different curves show the profiles of ﹩2\,{x}_{{{\rm{H}}}_{2}}﹩ (solid), ﹩{f}_{{\rm{sh}}}\left({N}_{{{\rm{H}}}_{2}}\right){e}^{-{\tau }_{d}}﹩, and ﹩{f}_{{\rm{sh}}}\left({N}_{{{\rm{H}}}_{2},{\rm{tot}}}-{N}_{{{\rm{H}}}_{2}}\right){e}^{-\left({\tau }_{d,{\rm{tot}}}-{\tau }_{d}\right)}﹩ (dashed), from the different iterations indicated by the line colors.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Binned detection rates as a function of H I column density for the observational sample and our model.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: H2 mass-weighted histogram. Orange dashed contours delineate a constant ratio of dust-grain to gas-phase H2 formation, assuming a constant CR ionization rate of ζ = 10−16 s−1 and solar metallicity. Pink contours delineate a constant ratio between the collisional dissociation and photodissociation rates of H2.
Paper: Coronal Mass Ejections Deflected by Newly Emerging Flux: A Combined Analytic and Numerical Study
Authors: Yuhao Chen, Chengcai Shen, Zhixing Mei, Jing Ye, Jialiang Hu, Zehao Tang, Guanchong Cheng, Shanshan Xu, Abdullah Zafar, Yujia Song, Jun Lin
Figure caption: Equilibrium evolution as the NEF strength S increases quasi-statically, given yd = 2.5 and r00 = 0.05. From left to right, the columns show cases with the NEF fixed at xd = 4, 4.704, and 7. The top row plots the horizontal equilibrium position xh(S); the bottom row plots the height yh(S). Black curves are equilibrium branches. Dots denote the critical points where catastrophe occurs: purple for S* < 0 and orange for S* > 0. Orange stars mark a second equilibrium that may be reached after the loss of the original equilibrium at the same S*; the orange dashed line indicates S = S*. Insets in bottom panels illustrate the magnetic configuration at the corresponding critical states; border colors match those for critical points. These critical configurations are used as the initial conditions for the following MHD simulations.
Paper: Coronal Mass Ejections Deflected by Newly Emerging Flux: A Combined Analytic and Numerical Study
Authors: Yuhao Chen, Chengcai Shen, Zhixing Mei, Jing Ye, Jialiang Hu, Zehao Tang, Guanchong Cheng, Shanshan Xu, Abdullah Zafar, Yujia Song, Jun Lin
Figure caption: The top panels show the magnetic energy Eh (Equation (1)) of the system as a function of the flux-rope position (xh, yh) around the critical points: (a) a successful eruption (or CME) with S < 0 and xd = 7; (b) a failed eruption with S > 0 and xd = 4. Background shading and white contours show normalized Eh, the white “+” marks the critical equilibrium, and orange dots trace the simulated trajectory of the FR center. The bottom panels display the deflection angle θ vs. xd for these two cases: (c) S < 0 and (d) S > 0. The black curves are theoretical angle profiles: the solid curve is θsteep (steepest-decrease direction of Eh at the critical point), and the dashed curve is θeq (direction from the critical point to the secondary equilibrium). Orange symbols denote eruption modes from simulations: up-pointing triangles (one-step), circles (two-step), and down-pointing triangles (failed). In panel (d), we plot −θ for sign consistency. Overall, simulated CME deflections follow θsteep, whereas failed eruptions align with θeq.
Paper: Coronal Mass Ejections Deflected by Newly Emerging Flux: A Combined Analytic and Numerical Study
Authors: Yuhao Chen, Chengcai Shen, Zhixing Mei, Jing Ye, Jialiang Hu, Zehao Tang, Guanchong Cheng, Shanshan Xu, Abdullah Zafar, Yujia Song, Jun Lin
Figure caption: Trajectories of the flux-rope center. The top panels show the spatial x–y path, while the bottom panels present the temporal y–t evolutions. The left and right columns correspond to NEF with S < 0 and S > 0, respectively. Different locations (xd) are texted to the corresponding results. Blue, orange, and red profiles at the bottom represent one-step, two-step, and failed eruptions, respectively.
Paper: The First LWA Swarm Calibrator Survey
Authors: C. A. Taylor, G. B. Taylor, J. Dowell, S. Pezzaioli
Figure caption: Delay drift comparison between the right and left circular polarization after global fringe fitting. Points represent the median value within the first and third quartiles, denoted by the range bars. Note that the comparative delay is stable until approximately 1 hr before sunrise, where the ionosphere begins to ionize and the delay solutions diverge due to differential Faraday effects.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Relation between ΓPC and λEdd. Using an improper SE model, such as a blackbody, can falsely produce a strong positive correlation. When SE is instead modeled with a power law, the correlation vanishes. The most unbiased phenomenological model—the cutoff power law—yields only a marginal correlation (pnull = 2 × 10−2). Furthermore, when focusing separately on sources with ﹩{\mathrm{log}}\,{\lambda }_{{\rm{Edd}}}\lt -2﹩ or > −2, the correlation becomes insignificant in both cases. To better compare with historical literature, we present linear regressions assuming ﹩{\mathrm{log}}\,{\lambda }_{{\rm{Edd}}}﹩ as the independent variable.
Paper: Stellar Cycle Variability in Mount Wilson Stars and Dynamo Models: Rotation Rate and Dynamo Number Dependency
Authors: Suyog Garg, Rohan B. Mandrai, Bidya Binay Karak
Figure caption: Scatterplot between the parameterized variability and the rotational period for the B95+ set of stars. The variability class data are obtained from Table 5.3 in R. Egeland (2017). Stars are classified into different variability classes: either noncyclic “flat,” “long” (may have Pcyc > 20 yr), and “var” (highly variable); or cyclic “poor,” “fair,” “good,” and “excellent.” Stars with the small dot marker do not have a variability class. The rest of the layout remains the same as Figure 2.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Same as Figures 8 and 10, but with λEdd (Eddington-scaled UV luminosity multiplied by 2.75) replaced by the Eddington-scaled PC luminosity LPC,0.5−10/LEdd. The q correlation (top panels) weakens by ∼1σ–2σ (vs. Figure 8), while the ΓPC correlation (bottom panels) remains consistent within 1σ (vs. Figure 10).
Paper: Stellar Cycle Variability in Mount Wilson Stars and Dynamo Models: Rotation Rate and Dynamo Number Dependency
Authors: Suyog Garg, Rohan B. Mandrai, Bidya Binay Karak
Figure caption: Time series plots of MWO raw S-index data and the respective quasi-Planck fittings for the seven additional GK25 stars considered in this study. Two stars, HD 81809 and HD 166620, that have relatively well-defined cycles, and which were studied by S. Garg et al. (2019), are also shown for cycle comparison. Properties of the stars are tabulated in Table 2, while the fit parameters are given in Table 3.
Paper: A UV to X-Ray View of Soft Excess in Type 1 Active Galactic Nuclei. II. Broadband Correlations
Authors: Shi-Jiang Chen, Jun-Xian Wang, Jia-Lai Kang, Wen-Yong Kang, Hao Sou, Teng Liu, Zhen-Yi Cai, Zhen-Bo Su
Figure caption: Comparison of SE luminosity (left), SE strength (middle), and PC photon index (right) derived from different SE models. X-axes show results from zcutoffpl, while Y-axes show results from zbbody (blue) and zpowerlw (red). The black line marks the 1:1 relation; gray dashed lines show ±0.5 dex (or ±0.5 for photon index). Compared to zcutoffpl, zbbody underestimates SE and gives a softer PC; zpowerlw overestimates SE and gives a harder PC.
Paper: Stellar Cycle Variability in Mount Wilson Stars and Dynamo Models: Rotation Rate and Dynamo Number Dependency
Authors: Suyog Garg, Rohan B. Mandrai, Bidya Binay Karak
Figure caption: Same as Figure 4 but for evaluating the variability and Pcyc/Prot correlations. Only the stars that have the mean cycle period available in Table 2 are included.
Paper: Stellar Cycle Variability in Mount Wilson Stars and Dynamo Models: Rotation Rate and Dynamo Number Dependency
Authors: Suyog Garg, Rohan B. Mandrai, Bidya Binay Karak
Figure caption: Same as Figure 2 but for evaluating the variability and rotation period correlation of GK25+ set of stars using the quasi-Planck fit data.
Paper: Stellar Cycle Variability in Mount Wilson Stars and Dynamo Models: Rotation Rate and Dynamo Number Dependency
Authors: Suyog Garg, Rohan B. Mandrai, Bidya Binay Karak
Figure caption: Scatterplot between the parameterized variability (Equation (2)) and the inverse-squared Rossby number for the GK19 set of stars. The Spearman rank correlation r is also provided.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: The gray scatter of points in both panels are the N/O–O/H scatter for local measurements of N/O in H II regions (L. S. Pilyugin et al. 2012; D. A. Berg et al. 2020; N. S. J. Rogers et al. 2021, 2022), low-mass metal-poor galaxies (D. A. Berg et al. 2012, 2019; Y. I. Izotov et al. 2023), and CLASSY galaxies (K. Z. Arellano-Córdova et al. 2025a). These measurements demonstrate clearly the expected evolution of N/O based on low-ionization optical emission. The various ICF corrected variations of N/O that we calculated are distinguished by marker shape. The pentagons represent N+/O+, circles are N+2/O+2, and squares show N+3/O+2. The filled shapes are galaxies in our Low-z Sample, and the High-z Sample are plotted as unfilled shapes. The color bar gives the nhigh used in the calculations for the three-zone ne model. The histograms show the distributions of N/O and O/H values in each panel for the low z and high z, which are shown with black and white histograms, respectively. In each of these panels, the low-z outlier at high N/O is Mrk 996, which is being enriched by a large population of WN stars. Upper left: the uniform ne model described in Section 6 without ICFs. There is a clear discrepancy between literature scatter and most of our low-z and high-z measurements. Upper right: we plot the uniform ne model detailed in Section 6 with ICFs. We note that the discrepancy seen in the first panel is still present in the second one and is more severe for some points. Lower left: our new physical conditions determinations, described in Section 6, are used to calculate new direct gas-phase metallicities and N/O measurements, where possible, for both samples. Additionally, we include lines that demonstrate the median value for each type of N/O for ﹩{\rm{1}}2+\mathrm{log}({\rm{O}}/{\rm{H}})\lt 8.0﹩ in the Low-z (filled line) and High-z (unfilled line) Samples. These medians allow us to highlight that the High-z Sample has, on average, higher N/O than the Low-z Sample suggesting a redshift evolution in the derived N/O for all tracers. Note that we mark with dashed and dotted lines the changes between (b) and (c) for two objects, GN-z11 and Sunburst Arc, which we discuss further in Section 7. Lower right: we plot the maximum vector offsets for the each tracer of N/O for both the Low-z and High-z Samples between the uniform ne model with no ICFs and our multiphase with ICFs ne model. The N+/O+ measurements on average shift down and to the right. The N+2/O+2 measurements generally shift up and/or to the right for our recalculated values. The N+3/O+2 values change the most notably since these measurements require much larger ICFs across varying ﹩\mathrm{log}U﹩.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: We demonstrate that for our sample the ΣSFR correlates with both the ne and the different tracers of N/O that we measured. We plot the linear best fit for the ne–ΣSFR and N/O–ΣSFR relationships with a solid line and show the 3σ errors on the fit. Filled markers are galaxies in our Low-z Sample, while unfilled markers are galaxies from our High-z Sample. The ΣSFR clearly sorts all of our galaxies into the Low-z and High-z Samples since the High-z Sample has significantly higher ΣSFR than the Low-z Sample. Upper: we present the ne–ΣSFR for each measured ne in our sample. The color and marker shape distinguish the various measured ne, where green pentagons are the low-ionization ne, light blue circles are the intermediate-ionization ne, and dark blue squares are the high-ionization ne. We show the Pearson’s r correlation coefficient for all ne and low-, intermediate-, and high-ionization ne separately. Each of these p-values suggests a correlation between ΣSFR and ne except for the relationship between ΣSFR and the intermediate-ionization ne. Lower: we show the N/O–ΣSFR relationship for every measure of N/O that we obtained in this work. In this plot, the color and marker shape distinguish the various measured N/O, where green pentagons are the N+/O+, light blue circles are N+2/O+2, and dark blue squares are the high-ionization N+3/O+2. For N/O–ΣSFR, we only show the Pearson’s r correlation coefficient between all the N/O tracers and the ΣSFR. We find that the best linear fit for N/O–ΣSFR is not as steep as the relationship between ne–ΣSFR, but the correlation is tighter and less likely to be produced by two uncorrelated sets of data. Additionally, we note that the low-z outlier at high N/O is Mrk 996, which is known to be experiencing N enhancement from Wolf–Rayet stars.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: We explore the relationship between ne and various tracers of N/O. The color and marker shape distinguish the various measured N/O, where green pentagons are the N+/O+, light blue circles are N+2/O+2, and dark blue squares are the high-ionization N+3/O+2. Each N/O measurement is plotted against the ne used to calculate the emissivity for the N ion utilized in each measurement (i.e., N+/O+ versus nlow, N+2/O+2 versus nint, N+3/O+2 versus nhigh). While filled points show galaxies in our Low-z Sample, unfilled points are galaxies in our High-z Sample. As a precaution, we plot values that fall below the (conservative) sensitivity range as semitransparent. Specifically, in cases where the diagnostic ratio was greater than the low-density limit, we plot the densities as triangles. It is therefore clear that we are robustly tracing different ne in different ionization zones for the majority of our sample. We find that the overall increasing relationship between ne and N/O in this work can be described by a logarithmic fit. Note the outlier in this trend is Mrk 996, which is known to have Wolf–Rayet driven N enhancement.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: The redshift evolution of ne(C+2) and ne(N+3) for our Low-z and High-z Samples of galaxies. Our fits to this relationship for ne(C+2) and ne(N+3) are shown in solid light and dark blue lines, respectively. The light blue circles show ne(C+2) values, while the dark blue circles are ne(N+3) values. We include literature measurements of ne(C+2) from M. V. Maseda et al. (2017), D. A. Berg et al. (2019), and M. W. Topping et al. (2025a) as small light blue diamonds. Downward pointing triangles of any color are showing where the derived ne are upper limits. Additionally, we compare the ne,low − z trends derived by Abdurro’uf et al. (2024) and M. W. Topping et al. (2025a) as dotted and dashed lines. In the right panel, we show the sensitivity ranges of the diagnostics used in deriving low-, intermediate-, and high-ionization ne. We show that the intermediate- and high-ionization ne are higher than the low-ionization ne across all redshifts, and the higher-ionization ne diagnostics follow ∝(1 + z)1.5−2.0, which is similar to the trend for the low-ionization ne redshift evolution.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: The five different ICFs that we fit as a function of ﹩\mathrm{log}U﹩ are displayed in each row. Each is shown at a range of metallicities between 0.05 Z⊙ and 0.40  Z⊙ indicated by the color bar in the upper leftmost tile. The shaded region that corresponds to a spread in burst age (t = 106.0–107.0 Myr). Every column corresponds to a different constant from ne = 102–106 cm−3. Row 1: N+/O+ is a fairly good estimate of relative N/O. Row 2: N+2/O+2 shows that this ionic abundance is overestimating N/O at low ionization parameter and underestimating it at high ionization parameter. Row 3: N+3/O+2 is underestimating N/O across the entire range of ionization parameters we consider, but most notably so at low ionization. Row 4: the (N+ + N+2)/(O+ + O+2) ICF is underestimating relative N/O at all ionization parameters, but this is most severe at high ionization. Row 5: finally, the (N+2 + N+3)/O+2 seems to infer relative N/O very well at log(U) > −2.75.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: Left: density inferred from a given density diagnostic emission line ratio versus the volume fraction of high-density gas for a two-phase density model for a given ion, with low-density gas of 103  cm−3 and high-density gas of 105 cm−3. The true volumetric averaged density is plotted as the solid magenta line. In comparison, nebular density diagnostics measure lower densities with the low-ionization optical diagnostics severely biased to the low-density value for most of the fractional range, while the high-ionization UV diagnostics more closely trace the ne,avg due to their increased sensitivity to high-ne gas. Right: we compare the ne,infer for each diagnostic emission line ratio to the ne,avg to emphasize which ions serve as good tracers of the true ne,avg for an ionization zone with a multiphase density.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: Left: Te,high when assuming a constant ne compared to when a three-zone neis assumed. We find that the three-zone ne model produces lower Te,high than the constant ne model. Middle: comparing the gas-phase metallicities between these two models predictably shows that the three-zone ne model generates higher metallicities. Right: when looking at the UV log(N/O) derived in each model, we find that the three-zone ne model on average drives UV log(N/O) up for both our High-z and Low-z Samples.