adsabs/AstroCLIMB huggingface dataset:
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Orbit-averaged inspiraling timescale as a function of a b,0, given by Equation (20). Values are normalized to the analytical BH stopping time given in Equation (7). For ε  ρ  = 0.5, τ insp > 0, while for ε  ρ  = 2, τ insp < 0. A positive timescale corresponds to an orbital tightening, while a negative timescale corresponds to an orbital widening. An increase in the absolute value of τ insp is associated with a decrease in the rate of orbital tightening or widening. A least-squares fit to a power law of the form ﹩\propto {({a}_{{\rm{b}},0}/{R}_{a})}^{B}﹩ is performed. The shallow density gradient models (ε  ρ  = 0.5) are compared with the trend ﹩{({a}_{{\rm{b}},0}/{R}_{a})}^{0.19}﹩ found by A. Antoni et al. (2019). For the case where ε  ρ  = 2.0, ﹩{\tau }_{\mathrm{insp}}\propto {({a}_{{\rm{b}},0}/{R}_{a})}^{-1.1}﹩. This implies that binaries embedded in steep stellar density gradients will soften at a rate that progressively increases as a expands.
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: The orbit-averaged frequency ﹩{\tau }_{\mathrm{insp}}^{-1}﹩ in the (a b,0,ε  ρ ) plane for a binary with q = 0.15. ﹩{\tau }_{\mathrm{insp}}^{-1}﹩ provides an estimate of the ratio between the change in binary separation Δa b averaged over an orbital period and the initial separation a b,0. The orbit-averaged frequency ﹩{\tau }_{\mathrm{insp}}^{-1}﹩ is selected here to better illustrate cases that, over the duration of the simulation, show no appreciable change in their separation. For such cases, ﹩{\tau }_{\mathrm{insp}}^{-1}\approx 0﹩. Values in the colorbar are given in units of the analytical BH stopping time given in Equation (7). The pink-colored values show binaries that are tightened by the interaction with the CE flow (﹩{\tau }_{\mathrm{insp}}^{-1}\gt 0﹩), while blue colors indicate binaries that become less gravitationally bound (﹩{\tau }_{\mathrm{insp}}^{-1}\lt 0﹩). The darker colors mark binaries that experience a larger change in Δa b over an orbital period. The white symbols show cases where Δa b ≈ 0 within the simulation errors, and thus mark the transition between binary hardening and binary softening.
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Common envelope flow conditions during the assembly of PSR J0337+1715. ε  ρ  (top panel) and ﹩{{ \mathcal M }}_{\infty }﹩ (bottom panel) are each shown as a function of the radius from the center of mass of the primary during the asymptotic giant branch. The yellow line represents the radius at which a 1 M ⊙ Sun-like star will become tidally disrupted, while the orange line shows the tidal disruption radius for the embedded binary (a b,0 = 60R ⊙). The red line shows the CE onset boundary as defined in M. MacLeod & A. Loeb (2020), implying that most of the material above this line will be lost before CE sets in.
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Stopping timescale for a binary with q = 0.15, embedded in a CE flow of varying physical conditions. Values are normalized by τ stop, BH as in Equation (7). The colors represent the different values of the density gradient parameter: ε  ρ . The trend shows that the stopping timescale of the center of mass of the binary decreases as ε  ρ  increases, so the center of mass of the binary will spiral in faster into the CE. We find τ stop to remain fairly constant regardless of the initial separation of the binary.
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Flow morphology around the binary for the suite of simulations used in this study. Colormaps show the density of the flow in the orbital plane. The three different columns from left to right show the change in semimajor axis: a b,0 = 0.16 (left), 0.42 (middle), and 1.0 (right). The three different rows show the change in the flow driven by changes in ε  ρ : 0.5 (top), 1.0 (middle), and 2.0 (bottom).
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: The evolution of binaries in the (ε  ρ , ﹩{{ \mathcal M }}_{\infty }﹩) plane using numerical results from the simulations presented in this study. The relation between ﹩{{ \mathcal M }}_{\infty }﹩, ε  ρ , and q (Equation (12)) is shown for q = 0.10 and q = 0.15 (gray lines). The blue (pink) symbols show cases where binaries harden (soften) as they interact with the CE flow.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: SGB selection and relevant isochrones. The left panel shows our initial SGB region selection colored by MUSE metallicity. The middle panel shows stars with –1.75 < [Fe/H] < −1.65 and isochrones (described in Section 4.2) with [Fe/H] = −1.7, and ages ranging from 5 to 15 Gyr (top to bottom) overplotted in green. The solid lines are the solar-scaled helium abundance isochrones and the dashed lines are the Y = 0.40 models. The right panel is similar to the middle, now with [Fe/H] = −1.0 and isochrones colored in red. Our selection utilizes the region where the models are the most similar.
Paper: The Rise of Nova V1674 Herculis
Authors: Robert M. Quimby, Brian D. Metzger, Ken J. Shen, Allen W. Shafter, Hank Corbett, Madeline Overton
Figure caption: Ratio of the ZTF g-band flux to a best-fit fourth-order polynomial fit from 2019 through t ref folded by the 501 s spin period (colored dots). The final, anomalously bright measurement prior to t ref is circled. The red curve shows a spline fit to the better-sampled but lower-amplitude ZTF r-band light curve for comparison. The gray crosses show the first three ASAS-SN detections divided by the best-fit three-phase toy model from Section 5.4, and the gray squares mark these same values shifted by 0.2 P WD.
Paper: The Rise of Nova V1674 Herculis
Authors: Robert M. Quimby, Brian D. Metzger, Ken J. Shen, Allen W. Shafter, Hank Corbett, Madeline Overton
Figure caption: Three-phase toy model fits (gray curves) to the ASAS-SN and Evryscope measurements. Black points are AAVSO measurements (B. K. Kloppenborg 2023), either visual or in the V band, which are plotted as equivalent to g-band fluxes assuming no systematic offsets and are not included in the fitting. Purple dots give the Fermi/LAT photon flux from K. V. Sokolovsky et al. (2023) arbitrarily scaled to align the last two detections with the AAVSO measurements. The time span covering the Fermi/LAT detections is highlighted, and limits are shown outside this range with downward-pointing arrows. The first reported epochs of optical spectroscopy are marked with an “S” (E. Aydi et al. 2021; U. Munari et al. 2021).
Paper: The Rise of Nova V1674 Herculis
Authors: Robert M. Quimby, Brian D. Metzger, Ken J. Shen, Allen W. Shafter, Hank Corbett, Madeline Overton
Figure caption: Historical ZTF g-band light curve (gray dots) compared to the earliest ASAS-SN (green Xs) and Evryscope (blue dots) detections. The orange dots are the magnitudes after stacking four consecutive Evryscope observations. The dashed line shows the best-fit three-phase toy model (see Section 5.4). The plot is truncated well below V1674 Her’s visual peak of 6.2 mag at about HJD 2459377.5 + 0.84 days to emphasize the early evolution.
Paper: The Rise of Nova V1674 Herculis
Authors: Robert M. Quimby, Brian D. Metzger, Ken J. Shen, Allen W. Shafter, Hank Corbett, Madeline Overton
Figure caption: Images centered on V1674 Her (top row), reference image model (middle row), and corresponding subtractions (bottom row) for select Evryscope observations on June 12 (UT). From left to right: first Evryscope limit (t EVR,0); first Evryscope detection (t EVR,0 + 8.2 minutes); early peak (t EVR,0 + 28.7 minutes); the dip (t EVR,0 + 34.9 minutes); and the first image after the Evryscope ratchet (t EVR,0 + 167.1 minutes). Each image is ﹩{30}^{{\prime} }\times {30}^{{\prime} }﹩ and has north up and east left. The red cross hairs mark the position of the nova.
Paper: The Rise of Nova V1674 Herculis
Authors: Robert M. Quimby, Brian D. Metzger, Ken J. Shen, Allen W. Shafter, Hank Corbett, Madeline Overton
Figure caption: Radius and temperature evolution of the best-fit three-phase toy model. Dashed lines mark the estimated, volume-equivalent Roche lobe radius, R Roche, and the outer disk radius, R out. Approximate temperature ranges where higher opacities are possible (depending on density) are indicated by the light-gray bands.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: Posterior probability. This shows our sampling of the log-likelihood for one star in our selection. Overplotted are the PDF quantile levels (in orange) and Gaussian-fit σ contours (in white), showing excellent agreement at the 1 and 2σ levels.
Paper: The Rise of Nova V1674 Herculis
Authors: Robert M. Quimby, Brian D. Metzger, Ken J. Shen, Allen W. Shafter, Hank Corbett, Madeline Overton
Figure caption: Polynomial fits to the AAVSO data (gray solid curve) and these data supplemented with the faster-rise portion of the Evryscope g-band light curve (dashed gray curve) suggest similar peak magnitudes (﹩{V}_{\max }\sim 6.2﹩ mag) and t 2 times of 1.01–1.08 days.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: The age–metallicity relation. Left: the age distribution of the SGB star sample in equal number (N * = 803) metallicity bins. The colors correspond to the color map of Figure 1. Right: the 2D histogram of stars in the age–metallicity plane is given by the color map, where purple is less dense and yellow is denser. The median uncertainty is given by the black contour in the lower center. The Gaia–Sausage/Enceladus SFH (G. Limberg et al. 2022) is shown by the orange line. On the right side we show the full [Fe/H] histogram with each equal number bin regions denoted by colored patches. On the top of both panels we show the full age histogram for the clean SGB sample.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: Left: mean age vs. [Fe/H] systematics. Our mean age (left) and age spread (right) as a function of metallicity with our fiducial results (black points) as well as systematic tests (colored points; marker labels shared with both panels). In both panels error bars show the 1σ uncertainties and gray bars along the top denote the [Fe/H] equal number bin edges. Generally, our systematics tests slightly affect the mean ages but not the trend with [Fe/H] except for the C + N + O abundance, which significantly impacts this measurement. The age spread is largely independent of any systematic effects.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: Left: mean age and age spread. Our mean age and deconvolved age-spread constraints are shown in black circles and blue boxes, respectively. The black points are located at the median [Fe/H] of the bin. Center age spread vs. [Fe/H]. The lower panel shows the metallicity histogram for our sample. The upper panel shows the age spread for each metallicity bin. The gray lines across the top delineate the extent of our equal number metallicity bins. Right: age spread vs. mean age. The contours are color coordinated with the left panel to indicate metallicity. We show the 2D 1, 2, and 3σ confidence levels from the MCMC fitting for these values. The age spread increases with age.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: SGB ages and age uncertainties. The full data set is shown by the gray points in all panels. Left panels: the initial selection is shown colored by the age with the top panel showing all stars with ages less than 12 Gyr and the bottom panel showing those with ages greater than 12 Gyr. Center panels: the reliable subsample after removing stars based on their age errors and systematics is shown colored by age. Right panels: the reliable subsample is shown colored by the age uncertainty via Gaussian fitting.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: SGB chromosome maps. Left panels: each star is colored by its age showing the distribution of old and young stars within the color–color space. Right panels: SGB chromosome map. Each star is colored by its metallicity. We see several distinct features (see text for more details) as well as discrete subpopulations, which will be the focus of future work.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: Derivation of an empirical reddening correction for ω Cen. All panels show the extinction-corrected ridgelines for two Milky Way globular clusters, NGC 4147 and NGC 7089 (magenta and cyan lines). The black line shows the dominant [Fe/H] ∼ −1.7 metallicity population in ω Cen shifted by different extinctions in each panel. The left panel shows the ridgeline with no extinction; the middle panel the ridgeline using the E(B  − V) from W. E. Harris (1996) of 0.12, while the right panel shows our best-fit E(B − V) = 0.185.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: C + N + O systematics. The consideration of the relation between C + N + O enhancement and [Fe/H] makes a noted difference in age determination, though still largely within 2 times the average age error. The turnover at [Fe/H] = −1.0 is due to the C + N + O relation being held at a constant value above this metallicity.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: Helium abundance systematics. Each point in our final selection is colored by the difference in age determination when considering helium-enhanced isochrones vs. solar. Our selection is limited to stars with a helium age difference of less than 2 times the average age error, which only removes 216 stars.
Paper: oMEGACat. IV. Constraining the Ages of Omega Centauri Subgiant Branch Stars with HST and MUSE
Authors: C. Clontz, A. C. Seth, A. Dotter, M. Häberle, M. S. Nitschai, N. Neumayer, A. Feldmeier-Krause, M. Latour, Z. Wang, S. O. Souza, N. Kacharov, A. Bellini, M. Libralato, R. Pechetti, G. van de Ven, M. Alfaro-Cuello
Figure caption: Mean age vs. age-spread systematics for F625W. Our mean age results are dependent on our choice of photometric band, though the age-spread values are typically in good agreement regardless. See Section 6.1.3 for more details.
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: MS stars binned by their companion WDs ages. The gray-shaded regions show the range of rotation periods spanned by f spot = 0, solar-metallicity gyrochrones launched from the median percentile of Upper Sco at the WD age bounds, which are plotted as black solid lines. Gyrochrones with f spot = 25% and f spot = 50% launched with the same P init at the same ages are plotted as black dashed and dotted lines, respectively, and the corresponding region of allowed rotation periods is shown in light pink and green. The vertical purple band represents the fully convective boundary. Stars are color coded by ∣ΔP rot/σ  w ∣ (see Section 4.2). Blue points show good agreement, while the redder points show worse agreement between the observed and the predicted rotation periods.
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 Upper Sco rotation distribution at 10 Myr (G. Somers et al. 2017) from which we adopt the initial rotation periods for the model tracks. The solid yellow line shows a 1D smoothing spline fit to the median rotation periods. This fit is evaluated at the stellar masses available in our model grid to compute their respective P init.
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: MS stars in the full wide WD+MS sample in T eff−P rot space. In all, 1985 rotation periods are retrieved from ZTF; 384 periods are from ATLAS; 102 periods are from Gaia DR3; K2 provides 82 periods; 78 periods are from ASAS-SN; 23 periods are retrieved from Kepler; 15 periods are from A. R. G. Santos et al. (2021); 20 periods are from A. R. G. Santos et al. (2020); 9 periods are from MEarth North, and 3 periods are from MEarth South. The most opaque markers represent the MS stars in the WD + MS binaries that made it into the final selection (185 systems) described in Section 3. The McQuillan Kepler field (A. McQuillan et al. 2014a) of 34,030 MS stars below 6500 K is shown in the background, together with the additional detection of 15,640 M- and K-type Kepler stars by A. R. G. Santos et al. (2019).
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 launched from the median percentile of the Upper Sco distribution of initial rotation periods are shown as a solid orange line in each plot against observed cluster member rotational sequences. These gyrochrones are fit to the cluster’s observed periods of stars that have converged onto the cluster’s rotational sequence. Shaded regions around each gyrochrone account for the uncertainty in the cluster’s age at which the models are being evaluated. Note that the values of P rot and T eff in these clusters do not span the same range.
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: ZTF stars from Y. L. Lu et al. (2022) are plotted as gray circles. Our gyrochrones are shown as solid lines and color coded by their age. The gyrochrones are constructed using a non-spotted solar-metallicity grid and launched from the median P init percentile in Upper Sco. For convenience, selected gyrochrones for a wide range of ages are provided in Appendix C.
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: Properties of the 185 binaries with precise WD ages in the sample. We distinguish fully convective (FC) MS stars from partially convective (PC) MS stars based on their absolute Gaia magnitude, M  G , and Gaia BP − RP color measurements using Jao's gap (W.-C. Jao et al. 2018).
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: Gaia color–magnitude diagram showing the sample of 185 WD + MS binaries with the most precise WD total ages (average uncertainty <10%). The W.-C. Jao et al. (2018) gap is shown as a solid black line.
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: Top: contribution of the cooling age to the total age of the WD as a function of mass. Bottom: WD total age as a function of mass; the uncertainties on the WD ages have been inflated by empirically determined factors (T. M. Heintz et al. 2022) to compensate for systematics on the total ages.