adsabs/AstroCLIMB huggingface dataset:
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Time-averaged mass flux (estimated using the hydrodynamic quantities) through the T = 0.5 MeV surface as a function of entropy for various resolutions (indicated as Nr × Nθ in the top-right corner).
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Average abundance per baryon for various values of electron fraction Ye used in the nucleosynthesis calculations to set the initial composition. The MHD simulation corresponding to these nucleosynthesis calculations has been run with the Helmholtz EOS for a nonrotating PNS with a polar magnetic field B0 = 4 × 1015 G (at a resolution of 256 × 128).
Paper: Establishing a Connection between the Jet and the Corona in Black Hole Low-mass X-Ray Binaries
Authors: Eric M. Davidson, Jaiverdhan Chauhan, Anne Lohfink, Thomas D. Russell, Rhaana Starling, Charlotte Johnson
Figure caption: Top panel: the corona heights of MAXI J1820+070’s 2018 outburst determined through X-ray spectral modeling. Bottom panel: the evolution of the jet’s radio spectral index during the same outburst. For this source we determine the radio spectral index by modeling radio flux values compiled by C. Echiburú-Trujillo et al. (2024) with a simple power law. Modeled heights and values of α change from black to red when α dips below −0.25, indicating a move toward optically thin values for the jet. Background shading represents the source’s spectral states taken from M. Shidatsu et al. (2019) and J. Homan et al. (2020). The vertical green line present in both panels indicates the date of the jet ejection according to C. M. Wood et al. (2021). Errors on heights are estimated from our MCMCs and are reported at 90% confidence for all epochs. In this and following figures, a radio measurement with no reported corona size indicates a lack of available NuSTAR data on that date. The spectral fits and residuals for each epoch are shown in Figure 4.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Low-Ia (red) and high-Ia (blue) APOGEE DR17 stars from the calibration sample of the S24 catalog in [Fe/Mg]–[Mg/H] space (left) and [Mg/Fe]–[Fe/H] space (right). Plotted abundances are the S24 ﹩{\mathrm{log}}(g)﹩-calibrated abundances. The sample selection criteria (see Section 2) for low-Ia plateau stars (“plateau sample”) analyzed in this work are indicated by the black lines. The four different [Fe/Mg]cc assumptions ([Fe/Mg]cc = −0.3, −0.4, −0.5, −0.6) tested in Section 3 are indicated by the horizontal lines.
Paper: Establishing a Connection between the Jet and the Corona in Black Hole Low-mass X-Ray Binaries
Authors: Eric M. Davidson, Jaiverdhan Chauhan, Anne Lohfink, Thomas D. Russell, Rhaana Starling, Charlotte Johnson
Figure caption: Top panel: observed corona heights of MAXI J1535−571 during its 2017 outburst. Bottom panel: the radio/IR spectral indices from T. D. Russell et al. (2019) for the same time period. An increase in corona at the time of jet ejections and the quenching of the compact jet is observed. Values of α and corona height are shaded red once the radio spectrum is α < −0.25. Background shading represents spectral states taken from S. Nakahira et al. (2018), L. Tao et al. (2018), and T. D. Russell et al. (2019). Green shading represents dates of jet ejection (T. D. Russell et al. 2019). The spectral fits and residuals for each epoch are shown in Figure 5.
Paper: Establishing a Connection between the Jet and the Corona in Black Hole Low-mass X-Ray Binaries
Authors: Eric M. Davidson, Jaiverdhan Chauhan, Anne Lohfink, Thomas D. Russell, Rhaana Starling, Charlotte Johnson
Figure caption: Top panel: observed corona heights of MAXI J1348−630 during its 2019 outburst, with background shading indicating the dates of spectral state transitions according to L. Zhang et al. (2020). Bottom panel: the radio spectral indices obtained by F. Carotenuto et al. (2021). Values of α and corona height are shaded red when α < −0.25. An increased corona height is observed around the time of both ejection events (indicated by green shading; F. Carotenuto et al. 2021). The spectral fits and residuals for each epoch are shown in Figure 6.
Paper: Establishing a Connection between the Jet and the Corona in Black Hole Low-mass X-Ray Binaries
Authors: Eric M. Davidson, Jaiverdhan Chauhan, Anne Lohfink, Thomas D. Russell, Rhaana Starling, Charlotte Johnson
Figure caption: The data and spectral model comprising each epoch of MAXI J1820+070’s 2018 outburst (top panels). Bottom panels show (Data-Model)/Error. Plots are rebinned for illustrative purposes.
Paper: Establishing a Connection between the Jet and the Corona in Black Hole Low-mass X-Ray Binaries
Authors: Eric M. Davidson, Jaiverdhan Chauhan, Anne Lohfink, Thomas D. Russell, Rhaana Starling, Charlotte Johnson
Figure caption: The data and spectral model comprising each epoch of MAXI J1535−571 2017 outburst (top panels). Bottom panels show (Data-Model)/Error. Plots are rebinned for illustrative purposes.
Paper: Establishing a Connection between the Jet and the Corona in Black Hole Low-mass X-Ray Binaries
Authors: Eric M. Davidson, Jaiverdhan Chauhan, Anne Lohfink, Thomas D. Russell, Rhaana Starling, Charlotte Johnson
Figure caption: The data and spectral model comprising each epoch of MAXI J1348−630 2019 outburst (top panels). Bottom panels show (Data-Model)/Error. Plots are rebinned for illustrative purposes.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Δ[X/Mg]med vs. AIa/Acc for all elements except Mg, our reference element. Small black points are Δ[X/Mg]med,obs values for individual stars (i.e., Δ[X/Mg]med calculated from the observed [X/Mg] of each star), and AIa/Acc is calculated from the six-element fit with assumed [Fe/Mg]cc = −0.4. Large black points show the median of the black points in 10 evenly sized bins between the minimum and maximum AIa/Acc values of the plateau sample, and their error bars indicate the uncertainty on each median from 1000 bootstrap resamplings. The thick black line shows the best-fit Δ[X/Mg]med,obs vs. AIa/Acc line and the slope value is reported by the black text in the bottom left of each panel. Small blue points show Δ[X/Mg]med,2proc (i.e., Δ[X/Mg]med calculated from the two-process prediction [X/Mg]pred = [X/H]pred − [Mg/H], where [X/H]pred is given by Equation (2), resampled to account for reported observational error) for each star and new AIa and Acc values derived from refitting to the new simulated [X/H]pred. The thick blue line is the best-fit line between Δ[X/Mg]med,2proc and refitted AIa/Acc; the slope value is reported by the blue text in the bottom left of each panel. The length of the error bar on the bottom right of each panel represents the mean observational error for each element. Observed abundances for Na, Cr, V, Co, and Ce below an upper limit were removed following the procedure outlined in Appendix A.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Linear abundances {Si/Mg} (left) and {Mn/Mg} (right) as a function of {Fe/Mg} (bottom axis) or, equivalently, AIa/Acc (top axis, using Equation (8) assuming [Fe/Mg]cc = −0.4). Large red (blue) points indicate the median {X/Mg}–{Fe/Mg} value of the low-Ia (high-Ia) sequences calculated from the calibration sample at fixed [Mg/H]. The solid lines connect the median points to indicate the two-process predicted linear abundance values. The median points and connecting lines are calculated for [Mg/H] = −0.5 (dark purple line) and [Mg/H] = −0.1 (peach line). The gray box encloses the plateau sample: bounds are set by the sample selection in [Fe/Mg] converted to linear abundances and the 0.5–99.5 percentile range (99% of the data) in {X/Mg}.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Slopes (top) and residual standard error (RSE, bottom) of the Δ[X/Mg]med vs. AIa/Acc plots as illustrated in Figure 8. The slope and RSE are calculated in 0.1 dex [Mg/H] bins centered at [Mg/H] = −0.1, −0.2, −0.3, −0.4, −0.5, to show the potential metallicity dependence of these quantities. Error bars in the top panel indicate the uncertainty on the slope from the linear regression covariance matrix; they are frequently smaller than the marker. The RSE in the bottom panel is calculated as the standard deviation of residuals from the linear fit. In both panels, filled triangles indicate the data (Figure 8, black lines) and the open circles indicate the two-process prediction with Gaussian observational errors (Figure 8, blue lines). Observed abundances for Na, Cr, V, Co, and Ce below an upper limit were removed prior to calculation of the slope and RSE following the procedure outlined in Appendix A.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Covariance matrix of residuals Δ[X/Mg] for stars on the low-Ia plateau. In the left panel, Δ[X/Mg] are the observed residuals from the median plateau value, i.e., Δ[X/Mg]med,obs as in Figure 8. In the right panel, Δ[X/Mg] are the two-process residual abundances as described in Equation (3), but with Mg used as the reference element (Equations (11)–(12)), and the covariance from measurement uncertainty has been subtracted. The α (Fe-peak) elements are highlighted by the purple (yellow) square in both panels. Blue filled circles and red open circles denote positive and negative values, respectively, with area proportional to the value of the covariance. Circles in both panels are on the same scale; for reference, in the left panel, the Na–Na circle is 0.03, O–O is 0.003, and Na–K is 0.000003.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Uncertainty in Acc, σ(Acc) (left); uncertainty in AIa, σ(AIa) (middle); and uncertainty in AIa/Acc, σ(AIa/Acc) (right) for stars in the plateau sample. For each star, we resample the abundances by drawing from a Gaussian distribution centered at the two-process predicted abundances from the multielement fit with width corresponding to the observational uncertainty. For each sample, we recalculate AIa and Acc; blue solid lines indicate that AIa and Acc were inferred from the six-element χ2-minimization procedure, while orange dashed lines indicate that AIa and Acc were calculated from only [Mg/H] and [Fe/Mg] using Equations (7) and (8). The uncertainty σ in AIa and Acc is the standard deviation of the recalculated AIa and Acc over 500 samples. Values were calculated assuming a plateau value of [Fe/Mg]cc = −0.4.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: [X/Mg] vs. [Mg/H] for all stars in the plateau sample, for all elements considered in this study (except the reference element Mg). The scale of the y-axis in each panel is the same, shifted only by a zero-point to best accommodate the core of each element’s distribution, so the level of scatter can be visually compared across all panels. The solid black line indicates the median value of [X/Mg], calculated in 0.1 dex wide [Mg/H] bins. The average observational uncertainty in [X/Mg] for each element, calculated by adding the [X/H] and [Mg/H] uncertainties in quadrature, are shown by the length of the error bars at the bottom right corner in each panel. Observed abundances for Na, Cr, V, Co, and Ce below an upper limit were removed following the procedure outlined in Appendix A.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption:  ﹩{q}_{\,\rm{Ia}\,}^{{\rm{X}}}﹩ (filled triangles) and ﹩{q}_{\,\rm{cc}\,}^{{\rm{X}}}﹩ (open circles) vectors as a function of metallicity for X = O, Ni, Mn, and Ce, derived from the full S24 calibration sample. Colors indicate different assumed plateau values, with increasingly light colors reflecting a decreasing [Fe/Mg]cc value (or increasing [Mg/Fe]pl); the colors match the lines depicted in Figure 1.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Box-and-whisker plot showing the distribution of the inferred ratio of SN Ia to CCSN contribution, AIa/Acc, using the two-process model for different assumed [Mg/Fe]cc, for the plateau sample defined in Section 2. The center horizontal line indicates the median, boxes indicate the interquartile (25th–75th percentile) range, and tails indicate the 5th–95th percentile range of the data. Acc and AIa are inferred using Equations (7) and (8) for the orange boxes. Acc and AIa are calculated using a χ2-minimization procedure to the six elements Mg, O, Si, Ca, Fe, and Ni as described in W22 and S24 for the blue boxes.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Δ[Si/Mg]med,obs (left) and Δ[Mn/Mg]med,obs (right) as a function of Δ[Fe/Mg]med,obs for the plateau sample. Panels share the same y-axis scale. Δ[Mn/Mg]med,obs shows the stronger correlation with Δ[Fe/Mg]med,obs in this figure because both elements have substantial SN Ia contribution, while Si does not.
Paper: Reconciling the Tension between Light-curve Modeling of Type II Supernovae and Neutrino-driven Core-collapse Supernovae Models with Late-phase Spectroscopy
Authors: Qiliang Fang, 其亮 方, Hiroki Nagakura, Takashi J. Moriya
Figure caption: Left panel: the optimized multiband light curves of SN 2014G at different fixed log Lprog, which are distinguished by colors. Middle panel: the median values and 68% CIs of the inferred EK (pink scatter points) and log MNi (green scatter points) from light-curve modeling as a function of fixed log Lprog. The black histogram represents the log Lprog distribution inferred from nebular spectroscopy. Right panel: the log Lprog-weighted distributions of EK (represented by the left y-axis) and log MNi (represented by the right y-axis). The contributions from EK (log MNi) distributions, with different fixed log Lprog, are distinguished by colors. The black dashed lines represent the median values of the distributions, and the black dotted lines represent the 16th and 84th percentiles.
Paper: Reconciling the Tension between Light-curve Modeling of Type II Supernovae and Neutrino-driven Core-collapse Supernovae Models with Late-phase Spectroscopy
Authors: Qiliang Fang, 其亮 方, Hiroki Nagakura, Takashi J. Moriya
Figure caption: Comparison between log Lprog and EK for SNe II in the sample. Left panel: comparison between log Lprog converted from nebular spectroscopy and the log Lprog-weighted EK. Right panel: comparison between log Lprog and EK inferred from light-curve modeling using wind models. Individual objects are distinguished by colors and markers. In both panels, the black scatter points are the results of core-collapse simulations. The regions surrounded by the black and red dashed lines represent the ranges of the models and observations respectively.
Paper: Reconciling the Tension between Light-curve Modeling of Type II Supernovae and Neutrino-driven Core-collapse Supernovae Models with Late-phase Spectroscopy
Authors: Qiliang Fang, 其亮 方, Hiroki Nagakura, Takashi J. Moriya
Figure caption: Comparison between log EK and log MNi for SNe II in the sample. Left panel: comparison between log Lprog-weighted log EK and log MNi. Right panel: comparison between log EK and log MNi inferred from light-curve modeling using wind models. Individual objects are distinguished by colors and markers. In both panels, the solid black points are the results of core-collapse simulations, and the region surrounded by the black dashed lines represents a rough estimation of their range. The transparent black points are the parametric SN models of F. R. N. Schneider et al. (2025). The log EK–log MNi relations from T. Müller et al. (2017; blue) and L. Martinez et al. (2022c; orange) are also plotted for comparison.
Paper: Reconciling the Tension between Light-curve Modeling of Type II Supernovae and Neutrino-driven Core-collapse Supernovae Models with Late-phase Spectroscopy
Authors: Qiliang Fang, 其亮 方, Hiroki Nagakura, Takashi J. Moriya
Figure caption: The dependence of inferred MHenv for SN 2014G from light-curve modeling based on fixed log Lprog (light blue scatter points). The black histogram is log Lprog independently estimated from nebular spectroscopy. The black and dotted solid lines are the log Lprog–MHenv relations of KEPLER models (T. Sukhbold et al. 2016) and MESA models with Dutch wind (wind efficiency η = 1; other parameters, such as mixing length and overshooting, are the same as the ones in the main text). The green box marks MHenv with an additional constraint from nebular spectroscopy, while the red box marks values favored by the wind models.
Paper: On the Origin of Abundance Variations in the Milky Way’s High-α Plateau
Authors: Tawny Sit, David H. Weinberg, Emily J. Griffith
Figure caption: Δ[X/Mg]med,obs vs. AIa/Acc, as in Figure 8, for elements significantly affected by upper limit removal (Na, V, Ce, Cr, and Co). Elements using the BAWLAS upper limit relations (C. R. Hayes et al. 2022) are in the top row while elements using the relations derived for dSph (M. Shetrone et al. 2025, in preparation) are in the bottom row. Measurements falling below the calculated upper limit for a given star’s Teff (Na, V, Ce) or Teff and SNR (Cr, Co) and subsequently removed from analysis in Section 4 are highlighted in red. The remaining stars are plotted in black.
Paper: Reconciling the Tension between Light-curve Modeling of Type II Supernovae and Neutrino-driven Core-collapse Supernovae Models with Late-phase Spectroscopy
Authors: Qiliang Fang, 其亮 方, Hiroki Nagakura, Takashi J. Moriya
Figure caption: Comparison between log Lprog–EK and log EK–log MNi for SNe II in the sample. This is the same as the corresponding figures in the main text except that the observed light curves are only corrected for E(B − V)MW.
Paper: Revising the Giant Planet Mass–Metallicity Relation: Deciphering the Formation Sequence of Giant Planets
Authors: Yayaati Chachan, Jonathan J. Fortney, Kazumasa Ohno, Daniel Thorngren, Ruth Murray-Clay
Figure caption: The radii and masses of the planets in our sample. The dotted and dashed lines show the mass–radius relation for pure H–He planets at 0.5 and 5 Gyr, respectively, for an incident flux of 108 erg s−1 cm−2.
Paper: Photometric Analysis of 30 Contact Binaries in M31
Authors: Xiang Gao, Kai Li, Li-Heng Wang, Hai-bo Yuan, Hong-rui Gu, Ya-Ni Guo
Figure caption: The M-R, M-L, and T-L distributions for contact binaries. The colored dotted lines indicate the evolutionary tracks for solar chemical compositions. The solid and dashed lines indicate the ZAMS and the TAMS, respectively. The gray filled and open circles represent the primary and secondary components of the contact binaries in the Milky Way, while the red filled and open circles represent those of the 30 contact binaries in M31.
Paper: Photometric Analysis of 30 Contact Binaries in M31
Authors: Xiang Gao, Kai Li, Li-Heng Wang, Hai-bo Yuan, Hong-rui Gu, Ya-Ni Guo
Figure caption: The relation between orbital angular momentum and total mass for contact binaries. The dashed line indicates the boundary line between the detached and contact binaries. The gray filled and open circles represent the primary and secondary components of the contact binaries in the Milky Way, while the red filled and open circles represent those of the 30 contact binaries in M31.
Paper: Photometric Analysis of 30 Contact Binaries in M31
Authors: Xiang Gao, Kai Li, Li-Heng Wang, Hai-bo Yuan, Hong-rui Gu, Ya-Ni Guo
Figure caption: Probability distributions of q, T2, i, f, L1g/LTg, L1r/LTr, L3g/LTg, L3r/LTr, λ, rs, and Ts determined by the MCMC modeling of M31_CB_16.
Paper: Revising the Giant Planet Mass–Metallicity Relation: Deciphering the Formation Sequence of Giant Planets
Authors: Yayaati Chachan, Jonathan J. Fortney, Kazumasa Ohno, Daniel Thorngren, Ruth Murray-Clay
Figure caption: Median estimates of the bulk metallicity for our planet sample assuming the metals are distributed uniformly throughout the planet (y-axis) and our fiducial choice (x-axis, MZ ≤ 10 M⊕ in the core, rest of the metals in the envelope).
Paper: Photometric Analysis of 30 Contact Binaries in M31
Authors: Xiang Gao, Kai Li, Li-Heng Wang, Hai-bo Yuan, Hong-rui Gu, Ya-Ni Guo
Figure caption: Probability distributions of q, T2, i, f, L1g/LTg, and L1r/LTr determined by the MCMC modeling of M31_CB_14.
Paper: Revising the Giant Planet Mass–Metallicity Relation: Deciphering the Formation Sequence of Giant Planets
Authors: Yayaati Chachan, Jonathan J. Fortney, Kazumasa Ohno, Daniel Thorngren, Ruth Murray-Clay
Figure caption: The left panel shows our metal mass measurements against planet mass, a sample of models from our fiducial model in blue, mean of the models in solid black, and the range of astrophysical scatter in dashed black lines. Solid straight lines show metal mass as a function of planet mass for a range of metallicities. The right panel shows the constraints obtained on the fiducial model parameters: core mass ﹩{M}_{{\rm{core}}}﹩, fraction of accreted material in metals fZ, and multiplicative term for the astrophysical scatter σmult.
Paper: Revising the Giant Planet Mass–Metallicity Relation: Deciphering the Formation Sequence of Giant Planets
Authors: Yayaati Chachan, Jonathan J. Fortney, Kazumasa Ohno, Daniel Thorngren, Ruth Murray-Clay
Figure caption: Bulk metallicity normalized by the stellar metallicity plotted against planet mass. Normalizing Zp by Z⋆ does not reduce the astrophysical scatter in our sample. Blue lines show fitted samples from our model of the form Zp/Z⋆ = a/Mp + b, where a = 2.6 ± 0.3 (for Mp in Jupiter masses) and b = 3.3 ± 0.5. The dashed black lines mark the range of the astrophysical scatter. A noteworthy difference between Zp/Z⋆ and Zp in Figure 6 is that outliers in Zp are less salient in Zp–Z⋆ space.
Paper: Revising the Giant Planet Mass–Metallicity Relation: Deciphering the Formation Sequence of Giant Planets
Authors: Yayaati Chachan, Jonathan J. Fortney, Kazumasa Ohno, Daniel Thorngren, Ruth Murray-Clay
Figure caption: Evolution models for a 0.3 MJup planet for different bulk metallicities assuming the metals are uniformly distributed inside the planet (i.e., no central core). The solid lines correspond to our updated evolution model. The models corresponding to the dashed lines are indicated in the panel titles. In the top left panel, we compare with models that use a solar-metallicity atmosphere but the same EOS for H–He and metals as our model. In the top right panel, we compare with models that use our adopted metal EOS and atmosphere models but with the SCvH EOS for H–He. In the bottom left panel, we compare with models that use ANEOS for metals. In the bottom right panel, we compare our evolution models with those calculated as in D. P. Thorngren et al. (2016).