adsabs/AstroCLIMB huggingface dataset:
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Evolution of the average rotation frequencies experienced by the g-modes (left) and the surface equatorial velocities (right) as a function of the two age indicators X c/X ini (top) and t/t MS (bottom). The evolution of the rotation rates are given with respect to the initial rotation rate at the zero-age main sequence. Different line styles correspond to different stellar masses: 2.5 M ⊙ (full), 5 M ⊙ (dashed), 7.5 M ⊙ (dashed–dotted), and 10 M ⊙ (dotted). Results for rigid rotation and no angular momentum transport are shown in blue and orange, respectively. Models with angular momentum transport from the Spruit–Taylor dynamo assuming an initial rotation rate of 10% Ωcrit are shown in green for comparison.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Left: spectroscopic ﹩{V}_{\mathrm{eq}}\sin i﹩ as a function of the asteroseismic V eq derived under the assumption of rigid rotation for the sample of SPB stars with space photometry. The size of the data points scales with the amplitude of the dominant dipole mode, while the symbols indicate whether the oscillations are retrograde (square), zonal (triangle), or prograde (circles) modes. Orange data points correspond to stars for which the ﹩{V}_{\mathrm{eq}}\sin i﹩ cannot be reconciled with the V eq values within the estimated errors. Right: derived inclination angles as a function of the azimuthal order. The data points have been slightly offset from the measured m value for the sake of visibility. The black horizontal line marks where i = 90°, i.e., the maximum inclination angle. Binary stars are indicated with open symbols.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Same as Figure 9 but for SPB stars observed from the ground. Stars with i < 20° are indicated in purple.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Core rotational frequency as a function of main-sequence age (top and middle panels) and surface gravity (bottom panels). The panels on the left-hand side show the results for the 33 SPB stars with space photometry, while the stars with ground-based data are shown on the right. Open symbols indicate known or suspected binaries. The four SPB stars with ground-based data for which the inclination angle is found to be inconsistent with the mode identification as discussed in Section 6 are marked in purple. The results are compared to the core rotation frequencies of ≈300 γ Dor stars derived by Li et al. (2020) in gray. The corresponding Spearman’s rank correlation coefficients r  s  and their p-values are indicated in the subplots.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Distribution of near-core rotation frequencies with age for the 33 SPB stars with space photometry (gray). Binary stars are indicated by open symbols. The vertical dotted lines show the dividing ages for the four different age groups G1–G4, and the black data points give the position of the average rotation and ages of each age group. The evolution of the near-core rotation for the case of rigid rotation (blue) and no angular momentum transport (orange) has been scaled to the average rotation and age in group G1. The same results assuming models with angular momentum transport from the Spruit–Taylor dynamo are shown in green for comparison.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Evolution of the average rotation frequencies (left) and the surface equatorial velocities (right) for a 5 M ⊙ star as a function of the two age indicators X c/X ini (top) and t/t MS (bottom), assuming angular momentum transport from the Spruit–Taylor dynamo (green). The intensity of the green lines for the Spruit–Taylor dynamo depends on the initial rotation rate as indicated in the legend. The two cases of no angular momentum transport (orange) and solid body rotation (blue) are shown for comparison.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Expected ranges of observed near-core rotation frequencies as predicted for the sample of SPB stars assuming rigid rotation (blue) and no angular momentum transport (hatched orange). The predicted regions are shown separately for the 33 stars with space photometry (left) and 13 stars with ground-based data (right) that have measured X c/X ini and t/t MS values. SPB stars that show an inconsistency between the derived inclination angles and mode identification are shown in purple. See Figure 7 for further explanations of the figure details.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Core rotational frequency as a function of main-sequence age (top) and surface gravity (bottom) for 34 γ Dor stars (pink), which have been modeled asteroseismically. The ≈300 γ Dor stars from Li et al. (2020) are once again shown in gray, and the Spearman’s rank correlation coefficients r  s  and their p-values are indicated in the subplots.
Paper: Short GRB Host Galaxies. I. Photometric and Spectroscopic Catalogs, Host Associations, and Galactocentric Offsets
Authors: Wen-fai Fong, Anya E. Nugent, Yuxin Dong, Edo Berger, Kerry Paterson, Ryan Chornock, Andrew Levan, Peter Blanchard, Kate D. Alexander, Jennifer Andrews, Bethany E. Cobb, Antonino Cucchiara, Derek Fox, Chris L. Fryer, Alexa C. Gordon, Charles D. Kilpatrick, Ragnhild Lunnan, Raffaella Margutti, Adam Miller, Peter Milne, Matt Nicholl, Daniel Perley, Jillian Rastinejad, Alicia Rouco Escorial, Genevieve Schroeder, Nathan Smith, Nial Tanvir, Giacomo Terreran
Figure caption: Bottom: r-band host luminosities vs. redshift for 73 short GRBs with redshifts and r-band magnitudes color coded by Gold, Silver, and Bronze samples (circles). Two bursts with limits on a coincident host and known redshifts from their afterglows are also shown (gold triangles). Approximate limits of the ground-based catalog (﹩{m}_{\mathrm{lim}}\approx 26﹩ mag) and HST sample (﹩{m}_{\mathrm{lim}}\gtrsim 27﹩ mag) are plotted as dashed lines. For the subset of bursts that lack a coincident host to ≳27 mag, these searches are sensitive enough to rule out the faint end of the observed short GRB host luminosity function to z ≈ 2, as well as the fainter end of the field galaxy population (grayscale; COSMOS; Laigle et al. 2016). Also shown are 85 long GRB host luminosities over the same redshift range (black circles; Savaglio et al. 2009; Svensson et al. 2010; Hjorth et al. 2012; Vergani et al. 2015; Blanchard et al. 2016), the host galaxy of the long GRB 211211A which has a likely kilonova (purple star; Rastinejad et al. 2022), the host galaxy of the possible short GRB-EE, GRB 060614 (green star; Gal-Yam et al. 2006), and the host of GW170817, NGC4993 (red star). Overall, short GRB hosts exist in more luminous galaxies than long GRBs at the same redshifts (although there is substantial overlap in their luminosity functions). Top: cumulative distribution of redshifts for short (black) and long (blue) GRBs.
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: The model distributions from Method 2 (product of the SNR surface density functions and selection functions: A ρ SNR(R)f sel(d, l)), with black contours at 0.5, 1.5, 2.5,… kpc−2. The numbers in each panel correspond to the model numbers in Table 3. The 1.0425 × 1.0425 kpc green squares represent the observed number of SNRs contained in each area according to the color bars at the left of each panel. The red circle indicates the GC, and the yellow circle indicates the Sun. The panel numbers correspond to the model numbers given in Table 3.
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Positions of Galactic SNRs from Table 1 projected onto the Galactic plane. The black circles show the positions of the SNRs. The concentric green rings (i: numbered in green) are at radius multiples of 1.0425 kpc centered at the GC (red circle), and the blue rings (j: numbered in blue) are at radius multiples of 1.0425 kpc centered at the Sun (yellow circle). The yellow shaded regions show examples of the label system.
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Top: the surface density distribution estimated from Method 1. The dashed red line is the best-fit line to SNR surface densities <9 kpc, the green solid line is the best-fit line omitting only the surface densities between 1.0425 and 3.1275 kpc, and the violet dashed–dotted line omits the first three bins. Bottom: the distribution of the predicted total number of SNRs in each ring.
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: H I spectrum of the SNR G51.26 + 0.11. Top: H I emission spectra (source: black; background: red). Bottom: source–background difference (blue). The ± 2σ noise level of the difference is shown by the dashed lines.
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: The black circles are the positions of observed SNRs, and the violet triangles are positions of a simulated set of 1050 SNRs (Method 1). The ring radii are in multiples of 1.0425 kpc.
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: The observed Galactic SNR densities (uncorrected).
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Examples of the  B  field configuration in the −M0 (dipolar) and −M1 (quadrupolar) model. The left and middle panels show the field direction projected on planes parallel to the midplane, displaced above and below midplane by 1.25 kpc. The right panel shows the field on a plane perpendicular to the midplane, through a position (x = −8.1 kpc, y = 0, z = 0) normal to the radial direction, roughly corresponding to the position of the observer for the computation of the RM Figures 18–20. The  B  field model is for a generic spiral galaxy; it has not been fitted to the Milky Way, so the scales on the axes are representative. Unlike Figures 18–20, the field is not integrated along the line of sight nor projected on the sky; these panels merely illustrate sections through the model. The background color shows the magnitude of the field (∣ B ∣), with a logarithmic scale. The field is neither symmetric nor antisymmetric about the midplane.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Constant latitude binned slices through the −M0–M1 model. The upper panel covers latitudes +35° < b < +40°; the red and blue curves are copied from the upper panel of Figure 2. The lower panel is for −45° <b < −40° corresponding to Figure 6. Error bars show the scatter of values in each longitude bin, which are necessarily small because of the low angular resolution of the model.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: The preferred model RM distribution resulting from a halo field configuration including −M0 dipolar and −M1 quadrupolar components. The model is arbitrarily rotated in longitude. Latitudes − 20° < b < + 20° are blanked. Latitude ranges used to compute the azimuth dependence shown in Figure 20 are indicated by dashed green lines.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Two examples of the distributions of values in longitude bins, both for the range 35° < b < 40°, with the GMIMS histogram in red and the extragalactic in blue. The upper panel shows the distribution of samples in the longitude bin from 340° ℓ < 350°, the lower panel shows the same for the bin from 50° < ℓ < 60° that includes part of the North Polar Spur. In both cases, the medians have been subtracted from the values, so that all the histograms have zero median. The rectangles at the top show the range from the 16th to the 84th percentiles, which we use to determine ±1σ for the error bars in Figure 2 and for the determination of ﹩{\chi }_{\nu }^{2}﹩ in Table 5.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Comparing the fitted values of coefficient C 2 (Equation (1)) at different latitudes for different bin widths, 4° and 15°, as in Figure 22. Only latitudes giving values of C 2 > 5σ are shown. For all but one point, the results agree within error bars of ±1σ. From this and similar comparisons with many different bin widths, we conclude that the bin size has minimal effect on the least-squares fitting in Section 2.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Comparing the fitted values of coefficients C 1 and C 2 (Equation (1)) at northern latitudes (15° < b < 55°) for 10° bins using the gridded extragalactic RMs vs. binning the extragalactic sources directly from Taylor et al. (2009). The left panel uses all sources with equal weighting. The right panel uses only the sources with the highest precision in RM, i.e., those with measurement error σ RM < 5 rad m−2.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Illustration of the effect of changing the bin width in longitude from 15° (24 bins, top panel) to 4° (90 bins, lower panel). Although there is more structure in the data on scales of a few degrees with the smaller bins, the results from fitting sine curves are changed only slightly.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: The correlation between RMs from the two surveys as a function of the bin widths. There is a small but significant reduction in the correlation coefficient as the bins get smaller.
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption: (a)–(c) SEM-BSE images of typical NanoSIMS analysis pits. (a) Iron-nickel analysis pits (white arrows) with 3 × 3 μm2 nominal size formed by ∼500 pA O− primary beam (MET 00526, chondrule b1). (b) Iron-nickel analysis pits (black arrow) with 6 × 6 μm2 nominal size formed by ∼75 pA O− primary beam (DOM 08006, chondrule b49). (c) Aluminum–magnesium analysis pits (black arrows) with 6 × 6 μm2 nominal size formed by ∼12 pA O− primary beam (QUE 97008, chondrule b15). (d) and (e) BSE images of chondrule b49 from DOM 08006. (f)–(h) Ion images from the area indicated in (e). Each ion image is 6 × 6 μm2. Dotted lines in (g) and (h) indicate the area of signal integration for quantification of isotope measurements. Abbreviations: Ol = olivine, An = anorthite, En = enstatite, Ca-px = calcium-rich pyroxene, Mes = mesostasis, Fe-ox = iron oxide, Fe-sul = iron sulfide.
Paper: Flexible Models for Galaxy Star Formation Histories Both Shift and Scramble the Optical Color–Mass-to-light Ratio (M/L) Relationship
Authors: Yijia Li, 轶佳 李, Joel Leja
Figure caption: The rest-frame (r − i) color may significantly reduce the uncertainty of M */L estimates from CMLR. Left: sSFR drives the correlation between (r − i) and ﹩\mathrm{log}(M/{L}_{g})﹩ residuals calculated from the mode of the HBM relationship. The Pearson correlation coefficient is 0.44. Right: the linear fit of ﹩\mathrm{log}(M/{L}_{g})﹩ upon both (g − r) and (r − i) has smaller scatter than the linear model using only (g − r). The shaded regions cover 1σ range of the residuals for the two linear models respectively. Both plots are based on the Prospector–α model.
Paper: Flexible Models for Galaxy Star Formation Histories Both Shift and Scramble the Optical Color–Mass-to-light Ratio (M/L) Relationship
Authors: Yijia Li, 轶佳 李, Joel Leja
Figure caption: The logarithmic density of galaxies on the (g − r)–﹩\mathrm{log}(M/{L}_{g})﹩ plane for the priors, the median of individual SED-fitting posteriors, and the median of each object after HBM shrinkage are shown in the left three columns respectively. The right column demonstrates the ﹩\mathrm{log}(M/{L}_{g})﹩ offset after and before the HBM shrinkage. The results shown here are based on the Prospector–α model. We observe a strong shrinkage effect for blue galaxies, but some red faint galaxies are pushed away from the average relationship.
Paper: Flexible Models for Galaxy Star Formation Histories Both Shift and Scramble the Optical Color–Mass-to-light Ratio (M/L) Relationship
Authors: Yijia Li, 轶佳 李, Joel Leja
Figure caption: The color differences between the two models. The bottom panel shows the distribution of the (g − r) offsets between Prospector–α fits and the simple fits, where the majority of galaxies are redder in Prospector- α. In the top panels, we show example spectra of galaxies with the typical color difference and the extreme color difference, where g-band and r-band model photometries are shown in triangles. Comparison between the two columns in the top panels indicates that the model offset in the rest-frame color mainly comes from the nebula emission.
Paper: Flexible Models for Galaxy Star Formation Histories Both Shift and Scramble the Optical Color–Mass-to-light Ratio (M/L) Relationship
Authors: Yijia Li, 轶佳 李, Joel Leja
Figure caption: Comparison to the (g − i)–﹩\mathrm{log}M/{L}_{i}﹩ relationships presented by other works. The black solid line is Prospector–α median relationship from our HBM. The blue and pink shaded regions are the 1σ and 2σ ranges of the model posteriors respectively. The green line shows the relationship from Bell et al. (2003). The yellow line represents the relationship given by Taylor et al. (2011). These two are empirical relationships derived from SED fitting to data like our work. The Zibetti et al. (2009), Into & Portinari (2013) relationships are based on stellar evolution models.
Paper: Flexible Models for Galaxy Star Formation Histories Both Shift and Scramble the Optical Color–Mass-to-light Ratio (M/L) Relationship
Authors: Yijia Li, 轶佳 李, Joel Leja
Figure caption: Comparison of the Prospector–α fits to the HBM prediction after shrinkage for S/N ≥ 19 galaxies, S/N < 19 galaxies, and the entire sample. Galaxies before the shrinkage are indicated in black, and galaxies after shrinkage are shown in green. The error bars represent the median standard deviation of ﹩\mathrm{log}(M/{L}_{g})﹩ over all colors. The model does stronger shrinkage for low S/N galaxies.
Paper: Flexible Models for Galaxy Star Formation Histories Both Shift and Scramble the Optical Color–Mass-to-light Ratio (M/L) Relationship
Authors: Yijia Li, 轶佳 李, Joel Leja
Figure caption: The importance of different factors in predicting the ﹩\mathrm{log}(M/{L}_{g})﹩ difference between the simple and Prospector–α model. The age difference is the most important.
Paper: Flexible Models for Galaxy Star Formation Histories Both Shift and Scramble the Optical Color–Mass-to-light Ratio (M/L) Relationship
Authors: Yijia Li, 轶佳 李, Joel Leja
Figure caption: Comparison between the probability density function of the input mock data to the posteriors of their HBM fits. The recovered PDF is similar to the input one to high precision.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Solutions to the two-dimensional V-shape problem at final time t = 12 μs. Note that each point in the profile plot is every five data points on the grid in the y-direction. (a) Contour plots of species mass fractions and nuclear energy generation rate. Each pair of contour plots shows the Strang solution using VODE on the left and the trained DNN model on the right along the vertical dashed line. (b) Profiles along the vertical dashed line.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Illustrated overview of our machine-learning approach. The gray arrows indicate the steps involved in generating the training data, the blue arrows the training and validation process, and the orange arrows the testing phase.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Solutions to the planar problem at final time t = 12 μs using an machine-learning model trained using data from the V-shape problem. (a) Contour plots of species mass fractions and nuclear energy generation rate. Each pair of contour plots shows the Strang solution using VODE on the left and the trained DNN model on the right along the vertical dashed line. (b) Profiles along the vertical dashed line.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: (a) Profile of species mass fractions and nuclear energy generation rate at final time t = 12 μs, and (b) validation results using the negative inverse log form of X  k  as input for full DNN. Note that each point in the profile plot is every five data points on the grid in the y-direction.