adsabs/AstroCLIMB huggingface dataset:
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: The folded RV data and the normalized LCs in different bands using the period of 2.7735540 days. The vertical gray lines mark the phases of the inferior conjunction, quadrature, and superior conjunction. The RV data are calculated using the H α  line from LAMOST LRS (green dots) and MRS (red dots for S/N r  > 50; gray diamonds for S/N r  < 50).
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: Spectral disentangling with q = 2. The vertical panels show spectra in different phases (close to the minimum or maximum RV phase of the visible star). The blue lines mark the reconstructed spectra of the visible star, while the red lines represent the second component in each spectra. The green lines are the sum of the two components, and the black lines represent the observed spectra.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Electron flux spectra (cm−2 s−1 keV−1) for four different distances s from the loop apex: from top to bottom rows, s = 2.2 × 108 cm, 4.5 × 108 cm, 6.7 × 108 cm, and 8.9 × 108 cm (these correspond to distances of about one-fifth, two-fifths, three-fifths, and four-fifths of the way from the electron injection site at the loop apex toward the footpoint, respectively). The left column shows results for time t = 5 s (one-fourth of the way through the heating phase), the middle column shows results for t = 10 s (halfway through the heating phase) and the right column shows results for t = 20 s (end of the heating phase). The different curves in each plot are for different values of the turbulent conduction suppression parameter R, with α = 0 (Equation (2)) in all cases. The black dashed–dotted curves are for a collisions-only model obtained by setting the resistivity η equal to zero.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Temperature profiles at t = 10 s, 20 s (the end of the heating phase) and t = 40 s and t = 60 s, during the subsequent relaxation (cooling) phase. The top row is for the case α = 6, the second row is for the case α = 4, the third row is for α = 2, and the fourth row is for α = 0. The different curves reflect different values of R; the black dashed–dotted curves are for a collisions-only model obtained by setting the resistivity η to zero.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Velocity profiles at t = 10 s, 20 s, 40 s, and 60 s, for values of α from 6 (top row) to α = 0 (bottom row). The black dashed–dotted curves are for a collisions-only model obtained by setting the resistivity η to zero. Upward velocities are positive, and note the linear scale on the ordinate. For values of R > 0 the velocities are enhanced during the heating phase (first two columns), but suppressed during the relaxation phase (last two columns). The effects of turbulence are more enhanced for α = 0 than they are for α = 6.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Top two rows: overall (solid lines) and ohmic (dashed lines) heating rates (top row), and fraction due to ohmic heating (second row), as a function of position for the case α = 6, at times t = 0, t = 10 s, and t = 20 s. The different curves are for different values of the turbulent conduction suppression parameter R (Equation (2)). The black dashed–dotted curves are for a collisions-only model obtained by setting the resistivity η (and hence the ohmic heating rate Q ohmic) to zero. Bottom two rows: the same quantities, but for the case α = 0.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Pressure profiles at t = 10 s, 20 s, 40 s, and 60 s, for α = 6 (top row) and α = 0 (bottom row). The black dashed–dotted curves are for a collisions-only model obtained by setting the resistivity η to zero. For values of R > 0, the enhanced ohmic heating in the corona causes a significant pressure enhancement in the corona compared to the collisions-only (R = 0) case, so that the pressure profile is much more uniform. Note that the ordinate has a linear scale.
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: Comparison of J0606+2132 to other NS candidates. Top panels: histograms of systematic parameters for J0606+2132 and candidates. The blue and red histograms represent systems discovered by astrometry and RV, respectively. Black dashed lines mark the position of J0606+2132 in these histograms. Bottom panels: masses of visible stars vs. masses of the NS candidates (left panel) and eccentricities vs. orbital periods (right panel). Red and blue points represent the NSs discovered by RV and astrometry, respectively. The dots and squares represent systems where the visible stars are main-sequence stars and giants, respectively.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Loop-integrated heating rate ∫Q dz per unit area, for both collisions, ohmic, and total, for α = 6 (left) and α = 0 (right), normalized to the injected beam flux of 1011 erg cm−2 s−1. To avoid unnecessary clutter in the plots, only the cases R = 0 (zero turbulent scattering; collisions only) and R = 10 (strong turbulence) are shown.
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: H α  line profiles from LAMOST MRS observations plotted in different phases. The black lines show the mean spectrum of those MRS.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Density profiles at t = 10 s, 20 s, 40 s, and 60 s, for α = 6 (top row) and α = 0 (bottom row). The black dashed–dotted curves are for a collisions-only model obtained by setting the resistivity η to zero.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Loop-integrated X-ray spectra for α = 6 (top left), 4 (top right), 2 (bottom left) and 0 (bottom right). In each case, spectra for various values of R, from R = 0 (collisions only) to R = 10 are shown; the black dashed–dotted spectra are for a collisions-only model obtained by setting the resistivity η to zero. Both thermal and nonthermal contributions to the hard X-ray emission are included. For ease of presentation, the spectra for t = 10 s and t = 20 s are scaled upward by factors of 10 and 100, respectively.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: DEM profiles at t = 10 s, 20 s, 40 s, and 60 s, for values of α from 6 (top row) to α = 0 (bottom row). The black dashed–dotted curves are for a collisions-only model obtained by setting the resistivity η to zero.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. I. Results of Radiative Hydrodynamic Simulations
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: Results for different injected electron energy fluxes ﹩{{ \mathcal F }}_{o}﹩ (Equation (13)). From left to right: temperature vs. position, density vs. position, velocity vs. position, DEM vs. temperature (all cases are for α = 0 and at t = 20 s), and X-ray flux vs. photon energy for α = 0 and times t = 0, 10, 20 s. Top row: ﹩{{ \mathcal F }}_{o}=3\times {10}^{10}﹩ erg cm﹩{}^{{}_{2}}﹩ s−1; Middle row: ﹩{{ \mathcal F }}_{o}={10}^{11}﹩ erg cm﹩{}^{{}_{2}}﹩ s−1 (see Figures 4, 7, 6, 8, and 9, respectively); Bottom row: ﹩{{ \mathcal F }}_{o}=3\times {10}^{11}﹩ erg cm2 s−1.
Paper: Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264
Authors: Laurin M. Gray, Katherine L. Rhode, Catrina M. Hamilton-Drager, Tiffany Picard, Luisa M. Rebull
Figure caption: Measured v sin i vs. equatorial rotation velocity (V eq) for the 229 low-mass stars in NGC 2264 for which both were measured. Single stars and “possible” binaries are shown in blue and comprise the Main Analysis Sample. Objects we identified as “likely” binary systems are marked in yellow, and objects with v sin i  < 11 km s−1 are marked as upper limits with arrows. The magenta line marks v sin i = V eq, and the dashed green line marks v sin i = 0.785 V eq. A randomly distributed sample of stellar spin-axes is expected to have ﹩\langle \sin i\rangle ﹩= 0.785. For the Resolution-Limited Sample, we calculate ﹩\langle \sin i\rangle =0.784\pm 0.025﹩; this indicates that our sample of stars appears to have randomly distributed inclinations, and we don’t identify any systematic errors for our values adopted from the literature or our v sin i measurements.
Paper: Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264
Authors: Laurin M. Gray, Katherine L. Rhode, Catrina M. Hamilton-Drager, Tiffany Picard, Luisa M. Rebull
Figure caption: HR diagrams showing the Model Comparison Sample with isochrones (dashed yellow lines) and mass tracks (dotted black lines) from the starspot-free I. Baraffe et al. (2015) model (left) and the 51% starspot coverage G. Somers et al. (2020) model (right). The main sequence for both models is approximated by the 100 Myr isochrone (solid orange line). The color of the circles indicates the measured v sin i of the stars, with stars with v sin i or V eq below the 11 km s−1 velocity resolution limit represented by open circles. The vertical gray lines mark the main temperature-based subgroups that were also used in analysis. The stars mostly appear well above the 3 Myr isochrone from the I. Baraffe et al. (2015) models, seeming closer to 1 Myr. The stars are more scattered around the 3 Myr isochrone from the 51% starspot coverage G. Somers et al. (2020) models, which is comparatively cooler than the I. Baraffe et al. (2015) 3 Myr isochrone.
Paper: Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264
Authors: Laurin M. Gray, Katherine L. Rhode, Catrina M. Hamilton-Drager, Tiffany Picard, Luisa M. Rebull
Figure caption: Comparison of our v sin i measurements with measurements from R. J. Jackson et al. (2016; left) and E. J. Baxter et al. (2009; right). The error bars on the measurements from R. J. Jackson et al. (2016) are smaller than the markers. Objects with v sin i  < 11 km s−1 are marked as upper limits with arrows. Objects we identified as “likely” binary systems are marked in yellow, while “possible” binaries are in pink, and “single” stars are in blue. The magenta dashed line depicts a perfect one-to-one correlation. We find good agreement with the measurements from R. J. Jackson et al. (2016), but not with E. J. Baxter et al. (2009).
Paper: Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264
Authors: Laurin M. Gray, Katherine L. Rhode, Catrina M. Hamilton-Drager, Tiffany Picard, Luisa M. Rebull
Figure caption: Radius ratio of radius from v sin i and period measurements to radius predictions from models with different starspot coverage fractions, for 1 Myr (left), 3 Myr (center), and 5 Myr (right) models. Results are shown by temperature subgroup; all objects (pink diamonds), lower T eff group (purple downward-pointing triangles), mid T eff group (yellow squares), and upper T eff group (orange upward-pointing triangles). The I. Baraffe et al. (2015) model is shown with open symbols (only for 0% starspot fraction, as those models did not incorporate starspots), and the G. Somers et al. (2020) models use filled symbols. For all groups, radius inflation decreases as starspot fraction increases.
Paper: Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264
Authors: Laurin M. Gray, Katherine L. Rhode, Catrina M. Hamilton-Drager, Tiffany Picard, Luisa M. Rebull
Figure caption: Normalized v sin i distributions for stars we identified as “quality single stars” (blue) and “quality likely binary” systems in our analysis (yellow). Only objects with R TD ≥ 5 are included. The gray bar marks the area below the velocity resolution limit. The binary stars appear to rotate faster, on average, than the single stars.
Paper: Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264
Authors: Laurin M. Gray, Katherine L. Rhode, Catrina M. Hamilton-Drager, Tiffany Picard, Luisa M. Rebull
Figure caption: Normalized v sin i distributions for disked, CTTS stars (blue) and diskless, WTTS stars (yellow). The gray bar marks the area below the velocity resolution limit. The WTTS stars appear to rotate faster, on average, than the CTTS stars, and very few CTTS stars rotate faster than 50 km s−1.
Paper: JWST Validates HST Distance Measurements: Selection of Supernova Subsample Explains Differences in JWST Estimates of Local H 0 
Authors: Adam G. Riess, Dan Scolnic, Gagandeep S. Anand, Louise Breuval, Stefano Casertano, Lucas M. Macri, Siyang Li, Wenlong Yuan, Caroline D. Huang, Saurabh Jha, Yukei S. Murakami, Rachael Beaton, Dillon Brout, Tianrui Wu, Graeme E. Addison, Charles Bennett, Richard I. Anderson, Alexei V. Filippenko, Anthony Carr
Figure caption: Distance comparisons for NGC 5643 from multiple analyses. The SH0ES measurements can be found in R22 and A. G. Riess et al. (2024) for Cepheids, S. Li et al. (2024b) for JAGB, and here for JWST TRGB. Extragalactic Distance Database measurements are from G. S. Anand et al. (2022). The CCHP measurements can be found in W. L. Freedman (2021) and F24. All measurements are anchored to NGC 4258 in the first rung. We plot a consensus mean of μ = 30.52 ± 0.03 mag.
Paper: Toward a Unified Injection Model of Short-lived Radioisotopes in N-body Simulations of Star-forming Regions
Authors: Joseph W. Eatson, Richard J. Parker, Tim Lichtenberg
Figure caption: A comparison between the fraction of remaining disks and the fraction of high-mass stars that have not reached the end of their lives. Due to the relatively short disk lifetime most of the stellar disks have progressed to the planetesimal-formation phase before most SNae have occurred. The dotted vertical line indicates when the first stars with an initial mass under 25 M ⊙ undergo SNae, contributing to SLR enrichment according to M. Limongi & A. Chieffi (2018).
Paper: Toward a Unified Injection Model of Short-lived Radioisotopes in N-body Simulations of Star-forming Regions
Authors: Joseph W. Eatson, Richard J. Parker, Tim Lichtenberg
Figure caption: A series of violin plots detailing 26Al and 60Fe enrichment. Solar system enrichment is shown as a red dashed line; a value of Z 26Al,SS ≈ 5 × 10−5 is used for the 26Al graphs (K. Thrane et al. 2006), while a low value of Z 60Fe,SS = 10−8 and a high value of Z 60Fe,SS = 10−6 are used for 60Fe plots (H. Tang & N. Dauphas 2012; R. K. Mishra et al. 2016). The enrichment values are calculated at the point where the disk has “progressed” or at the end of the simulation, whichever is shortest. While there is a higher amount of 26Al enrichment, the primarily SNae-driven 60Fe enrichment is suppressed as most disks may not undergo SNae interaction.
Paper: Toward a Unified Injection Model of Short-lived Radioisotopes in N-body Simulations of Star-forming Regions
Authors: Joseph W. Eatson, Richard J. Parker, Tim Lichtenberg
Figure caption: A series of violin plots showing 26Al and 60Fe enrichment. Enrichment is calculated through the local model while disk progression is simulated in a similar manner to Figure 4. Solar system enrichment is shown as a red dashed line; a value of Z 26Al,SS ≈ 5 × 10−5 is used for the 26Al graphs (K. Thrane et al. 2006), while a low value of Z 60Fe,SS = 10−8 and a high value of Z 60Fe,SS = 10−6 are used for 60Fe plots (H. Tang & N. Dauphas 2012; R. K. Mishra et al. 2016). Compared to the global model SLR enrichment is significantly elevated; however, many simulations undergo no enrichment whatsoever with this model (see Table 1).
Paper: Toward a Unified Injection Model of Short-lived Radioisotopes in N-body Simulations of Star-forming Regions
Authors: Joseph W. Eatson, Richard J. Parker, Tim Lichtenberg
Figure caption: A comparison of cumulative yield of 26Al in stellar winds over 10 Myr from stars with a mass range of 20–60 M ⊙. The majority of the mass loss occurs near the end of each star’s life, as the star exits the main sequences and begins its Wolf–Rayet phase.
Paper: Toward a Unified Injection Model of Short-lived Radioisotopes in N-body Simulations of Star-forming Regions
Authors: Joseph W. Eatson, Richard J. Parker, Tim Lichtenberg
Figure caption: A plot of all simulations showing the fraction of all stellar disks that underwent any amount of enrichment from the local wind model vs. initial median local density. We observe a clear dependence on region density, which is more important than the number of stars in the region, despite simulations with a higher number of stars inherently having more massive stars.
Paper: Toward a Unified Injection Model of Short-lived Radioisotopes in N-body Simulations of Star-forming Regions
Authors: Joseph W. Eatson, Richard J. Parker, Tim Lichtenberg
Figure caption: A cumulative distribution function of final 26Al enrichment fraction (Z Al) for all disks grouped by subset with disk progression simulated. A significant population of disks have a higher enrichment fraction than the solar system upon entering the planetesimal-formation phase in the cases of systems with extremely large numbers of stars.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: CRIR map estimated from our parameter-inference algorithm. All grayed-out, hatched regions are estimated by our algorithm to have ζ > 5 × 10−13 s−1 and one or more of the following issues. The “X” hatching indicates regions where the estimated HCN or HNC abundance was below 10−12 with respect to hydrogen, and the dotted regions indicate locations where ﹩{X}_{\mathrm{HCN}}/{X}_{\mathrm{HNC}}\gt 4﹩, with the two appearing together when both conditions are true. White and black numbers indicate the number of transitions that are detected with S/N > 3 for a given region, and purple outlines indicate when there are no transitions above the J = 2–1 that meet this threshold. Gray contours signify HCN 1–0 emission at 1, 3, and 5 Jy km s−1 beam−1. Colored dots indicate the locations of recent star formation via radio continuum sources (supernova remnants and H II regions; J. S. Ulvestad & R. R. J. Antonucci 1997) and super hot cores (F. Rico-Villas et al. 2020). Note half of the unclassified sources are expected to be H II regions, and half are thought to be supernova remnants. The green circle in the bottom-right corner represents the ALCHEMI 1.″6 (∼28 pc) beam.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Comparison of our CRIR estimates with those from E. Behrens et al. (2022), J. Holdship et al. (2022), and V. H. M. Phan et al. (2024). As proxies for GMCs 2–10, which were not studied in this work, we provide values for regions 75, 58, 53, 47, 36, 26, 20, and 16, which are the regions that overlap most significantly with the plotted GMCs. The widths of the shaded regions at each data point indicate the most likely 66% of each ζ posterior distribution.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Probability density for HCN/HNC abundance ratio (a) and cosmic-ray ionization rate map (b) with dotted hatching in both plots corresponding to ﹩{X}_{\mathrm{HCN}}/{X}_{\mathrm{HNC}}\gt 4﹩.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Exponential moving average of the mean-squared-error loss as a function of training epoch calculated for both the training and validation data sets. Here, the neural network was trained for many epochs past our early stopping criteria (described in Section 3.1) to demonstrate the divergence between the training and validation set losses. The dashed gray line indicates the epoch from which the final weights would have been obtained, as the validation loss does not improve for more than 20 epochs after this point.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Schematic of our neural network architecture. Blue circles represent the nodes in the input layer of the neural network that contain our input parameters, purple circles represent the nodes that make up the neural network’s inner hidden layers, and the green circles represent the output nodes in the final layer, which contain the abundances for HCN and HNC, respectively.