adsabs/AstroCLIMB huggingface dataset:
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Comparisons of τ  cz  values as a function of mass (left panel) and effective temperature (right panel). We show our fiducial, solar-metallicity unspotted stellar models as a solid black curve. Models with identical physics but a 25% spot covering fraction are shown in gray. The N. J. Wright et al. (2018) empirical calibration is shown in purple, and the S. A. Barnes & Y.-C. Kim (2010) “global” model-based τ  cz  are shown in turquoise. Metal-rich ([Fe/H] = +0.2) models are shown as the dotted curve.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Comparison between the WD ages from this work and the median gyro-kinematic ages (Lu et al. 2021) for bins of Kepler stars around the MS stars in the sample. Data points are color coded by the effective temperature of the MS stars, with more transparent points indicating bins with at least 10 Kepler stars and more opaque points indicating bins with 30 or more Kepler stars. Uncertainties represent the upper and lower bounds on the WD ages, inflated as prescribed by Heintz et al. (2022). Histograms show the distributions of WD and gyro-kinematic ages.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: In the background, a 2D histogram shows the distribution of ΔP rot/σ  w  relative to the ages of WDs in a sample drawn from a synthetic population. Each bin is color coded based on the fraction of triples (i.e., the number of WDs in the bin that have had their age reset), while the transparency reflects the total count of WDs in the bin. Warmer colors signify a higher proportion of WDs merger products, and greater opacity indicates a larger overall WD count in the bin. The black circles represent the distribution of the observed sample. At young WDs ages, the observed sample exhibits an increased occurrence of systems with ΔP rot/σ  w  > 2 in a region prone to triple contamination, as indicated by the synthetic population.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Comparison between ∣ΔP rot/σ  w ∣ computed for the MS stars in our sample using [Fe/H] = +0.0 and [Fe/H] = +0.2 model grids. Stars are color coded by their observed rotation period. A 1:1 line is plotted as a black dashed line. The hatched region in the bottom-right corner highlights stars for which ∣ΔP rot/σ  w ∣ decreases to 3σ  w  or lower if a higher-metallicity model grid is adopted instead of a solar-metallicity one. Only a handful stars show improved values of ∣ΔP rot/σ  w ∣ when using an [Fe/H] = +0.2 model grid.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Kepler stars are color coded by their gyro-kinematic ages (Y. L. Lu et al. 2021) in grays. The MS stars in our sample are plotted as larger circles and color coded by the difference between the median of the gyro-kinematic ages of the neighboring binned Kepler stars and the age inferred from the WD companions. The dashed vertical line shows the T eff of the coolest star in the Kepler sample. MS stars for which age comparisons are not feasible due to an insufficient number of nearby Kepler stars are indicated with white circles. The typical uncertainty in T eff is shown at the top.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Solar-metallicity gyrochrones up to 10 Gyr constructed using three model grids with different spot covering fractions f spot. The sharp rise in rotation period occurs for the same 0.30–0.34 M ⊙ mass range across the three model grids; however, the location of this feature varies across a ∼350 K temperature window between the three model grids with different spot covering fractions.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: The sizes of the convective zone relative to the total size of the star in mass and radius coordinates as a function of time are plotted in the top and middle panels, respectively. The bottom panel shows the convective overturn timescale normalized by the solar value as a function of time. The black arrow shows the jump between partially convective (PC) and fully convective (FC) stars. In all panels, the saw-toothed curves represent stars undergoing fully convective episodes driven by nonequilibrium 3He burning (J. L. van Saders & M. H. Pinsonneault 2012a). All tracks have solar metallicity and a 25% spot covering fraction.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Contributions of the stellar mass M, radius R, luminosity L, photospheric pressure P phot, and convective overturn timescale τ  cz  factors to the total dJ/dt using solar-metallicity models with 25% spot covering fraction. The fully convective boundary is at M = 0.31 M ⊙.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Gyrochrones constructed using a metal-poor (left), a solar-metallicity (center), and a metal-rich (right) non-spotted model grid. We show gyrochrones for ages between 0.1 and 10 Gyr, with a step of 0.5 Gyr. While the location of the steep rise in P rot is shifted to slightly higher masses in metal-rich stars, the feature does not vary significantly in temperature and occurs at ≈3500 K across all model grids.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Left: rotation period as a function of effective temperature for a specific age, computed using a solar-metallicity model grid with f spot = 0%. Gray solid lines represent gyrochrones. Markers indicate stars undergoing nonequilibrium 3He burning. Right: the convective overturn timescale, normalized by the solar value, as a function of age for the same stars. Markers display τ  cz  at the corresponding ages shown in the left plots. The saw-toothed curves represent fully convective episodes. The jump in τ  cz  from the saw-toothed to the smooth curve marks the transition to a fully convective state. Once the stars become fully convective, they reach the peak of the P rot spike in the plot on the left.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Rossby number as a function of effective temperature as shown by solar-metallicity, f spot = 0% gyrochrones color coded by their age. At the fully convective boundary, highlighted in gray, the Rossby number sees a sudden decrease followed by a sharp increase over the span of ≈50 K.
Paper: Rotation at the Fully Convective Boundary: Insights from Wide WD + MS Binary Systems
Authors: Federica Chiti, Jennifer L. van Saders, Tyler M. Heintz, J. J. Hermes, J. M. Joel Ong, 加冕 王, Daniel R. Hey, Michele M. Ramirez-Weinhouse, Alison Dugas
Figure caption: Same as in Figure 19 but extended to older ages.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: The relationship between redshift dispersion σ and linear mass density μ where σ is determined using (left to right) the biweight estimator, the gapper, or a Gaussian fit. The gray contours in the top row show the distribution for all 13,200 segments, while those in the bottom row show the segments identified as “good” based on low bootstrap uncertainty σ err < 70 km s−1 and high Shapiro–Wilk statistic W > 0.98. From left to right, the number of segments included in the bottom row is 3624, 4245, and 2699. The dotted black line in each panel shows the result from the analytical model of D. J. Eisenstein et al. (1997). The relationship between dispersion and linear mass density is much tighter for the “good” segments, allowing us to use σ as a predictor for μ. It is also similar to the prediction from the analytical model.
Paper: A Buddy for Betelgeuse: Binarity as the Origin of the Long Secondary Period in α Orionis
Authors: Jared A. Goldberg, Meridith Joyce, László Molnár
Figure caption: Period–Wesenheit (P–W) luminosity relations for the OGLE-III LPVs in the LMC (gray), and for Galactic RSGs (blue) collected by L. L. Kiss et al. (2006) based on absolute J- and K-band magnitudes. Red points, from left to right, mark the positions of the O1, FM, and LSP periodicities for Betelgeuse. Darker gray points are semiregular and Mira variables pulsating in the FM and O1 modes. Thin dashed lines indicate various P–W relations for RGB, AGB, and Mira stars in the LMC from I. Soszyński et al. (2007).
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: Mock observation (left) and matter distribution (right) for one sample filament from the Millennium simulation. The filament is placed at a distance of 300 Mpc, corresponding to cz ∼21,000 km s−1. On the left, gray dots indicate the redshifts of galaxies with magnitude r < 19.5 within a wedge of thickness 2°. On the right, color indicates density, normalized to the average density of the Universe, within a thicker 4° wedge to show the context for these motions in terms of the underlying mass distribution. In both diagrams, the location of the large filament is clear, but it has a complex structure and is embedded in a network of smaller filaments.
Paper: A Buddy for Betelgeuse: Binarity as the Origin of the Long Secondary Period in α Orionis
Authors: Jared A. Goldberg, Meridith Joyce, László Molnár
Figure caption: Upper: phase offset between the RV and photometric variations. Classical Cepheids from Gaia DR3 (Gaia Collaboration et al. 2023b; V. Ripepi et al. 2023) are shown with pink and light gray points, while stars from R. Szabó et al. (2007) are shown with purple and dark gray for FM and O1 stars, respectively, for reference. LSP stars from C. P. Nicholls et al. (2009) are shown with dark blue symbols, whereas Gaia DR3 LSP candidates from Gaia Collaboration et al. (2023a) are given in light blue. The O1, FM, and LSP points for Betelgeuse are shown in red (from left to right). Lower: OGLE I-band LCs and RV curves folded with the LSP periods, including sine fits for selected stars from C. P. Nicholls et al. (2009), ordered by decreasing phase offset, with Betelgeuse inserted into the sequence. Selected stars are marked with black outlines in the upper panel.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: A detailed view of the same filament shown in Figure 1, illustrating the procedure for calculating redshift dispersions for overlapping segments along the filament. In the top panel, gray dots indicate the values of cz for individual galaxies, while blue points with error bars indicate the mean cz and standard deviation for overlapping segments of width 1°, with centers shifted by 0.°4. (In our analysis, we use segments shifted by 0.°2; here, we show half of them, so the galaxies are visible in the background.) The bottom three panels show the distribution of cz for three sample segments: from left to right, a segment with small σ and small σ err; a segment with large σ and small small σ err; and a segment with large σ and large σ err. Large values for σ err typically result from complicated structures like infalling groups or bifurcations in the filament.
Paper: A Buddy for Betelgeuse: Binarity as the Origin of the Long Secondary Period in α Orionis
Authors: Jared A. Goldberg, Meridith Joyce, László Molnár
Figure caption: We show the photometric (V-band and SMEI from M. Joyce et al. 2020; and from the AAVSO) and RV (T. Granzer et al. 2022) variations for the star, plus single sine fits with red dashed lines, using the same 2170 day periodicity. Importantly, dimming in Betelgeuse’s LSP always happens when the photosphere begins to move away from the observer, as indicated by the RV.
Paper: A Buddy for Betelgeuse: Binarity as the Origin of the Long Secondary Period in α Orionis
Authors: Jared A. Goldberg, Meridith Joyce, László Molnár
Figure caption: Schematic of the dust modulation by a companion as discussed in Section 4.8.3 over the course of an orbit. The diagram in the center shows four orientations of the companion (black circle) as well as Betelgeuse (solid red blob) and some circumstellar gas and dust (curly lines). The arrows represent the motion of the two objects. This is compared to the period in the LC (upper panel) and RV modulation (lower panel). The phase-folded data from Figure 2 are overplotted in gray, with the four highlighted phases labeled as A, B, C, and D. These approximately correspond to (A) the minimum brightness (increasing RV, with the stellar photosphere accelerating away from the observer), (B) increasing brightness (approximate RV maximum), (C) maximum brightness (decreasing RV, star accelerating toward the observer), and (D) decreasing brightness (minimum RV). The Great Dimming of 2020 can be seen in the phase-folded LC near LSP minimum (A). When α Ori B is behind Betelgeuse relative to the observer’s line of sight as indicated by the RV (configuration A), circumstellar dust is able to obscure the system. When α Ori B is in front of Betelgeuse (configuration C), dust unaffected by α Ori B is (at least partially) eclipsed by Betelgeuse.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: Median values and confidence intervals for the inferred value of the linear mass density based on the “good” segments in Figure 3. Dark blue points show the median values of ﹩\mathrm{log}\mu ﹩ for a given ﹩\mathrm{log}\sigma ﹩ with error bars from bootstrap resampling, and dashed lines show 16 and 84 percentiles (corresponding to 68% of the values, or one standard deviation). Solid dark blue lines show fits to the median points using a quadratic function. Table 1 shows the parameters for these fits, as well as the scatter given by the vertical distance between the median value and the dashed lines.
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: NICER and NuSTAR light curves for Epochs 1–4 (note that Epoch 2 does not have concurrent NICER observations). All the light curves have time bins of 100 s. The shaded parts of Epoch 1 and Epoch 3 light curves indicate the regions used for the joint spectral fitting described in Sections 3.1.2 and 3.3.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: Reconstruction of the linear mass density for the simulated filament in Figure 1 based on the values in Table 1. Gray lines show the actual mass density, while points with error bars show the values obtained from redshift dispersions, as measured using (from top to bottom) the biweight estimator, the gapper, or Gaussian fits. The vertical extent of the error bars corresponds to the “scatter” column in Table 1, and the horizontal extent of the caps on the error bars corresponds to the 1° (5 Mpc) segment length. Dark blue points are calculated using the top three lines of Table 1, while bold light green points are calculated using the bottom two lines of Table 1 for segments that qualified as “good” for 2.0σ clipping but not for 2.5σ clipping. The inclusion of 2.0σ clipping helps provide mass estimates for regions with lower densities.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: Illustration of the motions of galaxies in halos with M < 1013 M ⊙, for the same filament shown in Figure 1. The left panel shows the distribution of cz for all galaxies in the mock observations (gray) and for those in the limited range 18,000–24,000 km s−1(blue). The center panel shows the line-of-sight peculiar velocities for the galaxies in this limited range of cz, which would appear to be “in the filament” based on redshift. The right panel shows the peculiar velocities for all galaxies as a function of their position along the filament, with distance indicated by color. The bimodal pattern of positive peculiar velocities for foreground galaxies (dark purple) and negative peculiar velocities for background galaxies (light yellow) shows that the galaxies that appear to be “in the filament” based on their redshifts are primarily falling in from either side.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: Infall toward the same sample filament as in the previous figure, as shown through the relationship between peculiar velocity and distance. Points show galaxies from the mock observations over the distances 244–345 Mpc. Infall is evident as positive peculiar velocities on the near side of the filament and the negative peculiar velocities on the far side. Our cz selection range 18,000–24,000 km s−1 is indicated by slanted dashed lines, and galaxies in that range are color-coded by cz, as shown in in the inset histogram. We can see that most of the infall region is included in the selected range of cz. Vertical lines indicate distances within 10 Mpc of the filament distance, approximately the region used to determine μ; this region includes 70% of the galaxies in the redshift selection range.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: The relationship between ﹩\mathrm{log}\sigma ﹩ and ﹩\mathrm{log}\mu ﹩ when μ is found using cylinders with radii of 5 Mpc, 10 Mpc, and 15 Mpc, and σ is found using the biweight estimator. To facilitate comparison, the fit to the median values for the 10 Mpc case is overlaid in each panel. Because filaments are not isolated and do not have well-defined boundaries, there is not an absolute relationship between ﹩\mathrm{log}\sigma ﹩ and ﹩\mathrm{log}\mu ;﹩ it depends on the region used to define μ.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: llustration of the motions of galaxies in halos with M > 1013 M ⊙, in the same format as Figure 8. In the right panel, each cluster appears as a vertical band of galaxies at approximately the same longitude and approximately the same distance (color). This case highlights the presence of substructures, in which motions are driven by the orbits within individual groups and clusters.
Paper: Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Mary Crone Odekon, Trevor W. Viscardi, Jake Rabinowitz, Brandon Young
Figure caption: The relationship between ﹩\mathrm{log}\sigma ﹩ and ﹩\mathrm{log}\mu ﹩ when the filaments are placed at distances ranging from 75 Mpc to 450 Mpc, and σ is found using the biweight estimator. To facilitate comparison, the fit to the median values for the 300 Mpc case is overlaid in each panel. The wedge shape and apparent magnitude limit are given in the upper left of each panel. The relationship found for the 300 Mpc case holds across this wide range of distances if the absolute magnitude cutoff and the physical segment size are held constant, despite the range of wedge shapes.
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: The MAXI per-day light curve of MAXI J1803-298 showing the period corresponding to the entire outburst with the dashed vertical lines being the times of the four NuSTAR observations reported.
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Schematic image of the Jet-MAD model. Left: zoom-in view around the BH. Protons and electrons inside the MADs emit 100 GHz radio, X-rays, and gamma rays via synchrotron radiation. Magnetic reconnection in the BH magnetosphere accelerates the electrons, and the electrons emit the photons via synchrotron radiation. These photons interact with each other, forming a blob consisting of the electron–positron pairs. This blob expands and becomes the jet material observed in radio galaxies. Right: zoom-out view around the jet dissipation region. Magnetic reconnection in the jet accelerates the electrons, which emit optical and X-rays via synchrotron radiation. Plasma is entrained into the jet from the ambient gas.
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: Left: model fit to the NICER+NuSTAR data of Epoch 1, where an additional tbabs accounts for the extra column of absorption linked to the obscurer responsible for the light-curve dips. Right: XSTAR table model grid is used instead of the additional tbabs. For both plots, the data and the different model components are shown as described by the labels. For each model component, one curve fits for the persistent spectra (green), and one for the dip spectra (brown).