adsabs/AstroCLIMB huggingface dataset:
Paper: Why Do Semianalytic Models Predict Higher Scatter in the Stellar Mass–Halo Mass Relation Than Cosmological Hydrodynamic Simulations?
Authors: Antonio J. Porras-Valverde, John C. Forbes, Rachel S. Somerville, Adam R. H. Stevens, Kelly Holley-Bockelmann, Andreas A. Berlind, Shy Genel
Figure caption: The stellar-to-halo mass relation colored by the quenched fraction (﹩{\mathrm{log}}_{10}\left(\mathrm{sSFR}\ \left[{\mathrm{yr}}^{-1}\right]\right)\lt -11.0﹩) using DARK SAGE fiducial. The black solid line shows the median binned by halo mass. The dashed lines enclose 68% and 95% of the data, respectively. The green arrows represent the mass growth of halos and stellar mass in three different (0.5 dex)2 bins in the stellar mass-to-halo mass space shown in dashed cyan boxes labeled “A,” “B,” and “C.” (The arrows’ x- and y- extents are ﹩d{\mathrm{log}}_{10}{M}_{h}/{\rm{\Delta }}t﹩ and ﹩d{\mathrm{log}}_{10}{M}_{* }/{\rm{\Delta }}t﹩ respectively, where we have chosen ﹩{\rm{\Delta }}t=10/\mathrm{ln}(10)﹩ Gyr, corresponding roughly to the timescale necessary for a halo to grow by 1 dex. For simplicity, the halo growth rate is taken from the fitting formula in N. Bouché et al. (2010), and the stellar mass growth is assumed to come from star formation only.) Within each bin, we sort galaxies according to the ratio of their specific star formation rate to the specific halo mass growth rate, i.e., (the arctangent of) the angle the arrow would make with the x-axis, and plot the average arrow derived from the upper and lower halves of the distribution. Galaxies in box A and B tend to increase the stellar mass scatter.
Paper: Why Do Semianalytic Models Predict Higher Scatter in the Stellar Mass–Halo Mass Relation Than Cosmological Hydrodynamic Simulations?
Authors: Antonio J. Porras-Valverde, John C. Forbes, Rachel S. Somerville, Adam R. H. Stevens, Kelly Holley-Bockelmann, Andreas A. Berlind, Shy Genel
Figure caption: Black hole mass as a function of halo mass for DARK SAGE (purple) and TNG (blue) galaxies. In all panels, the blue line is unchanged. The left panel shows fiducial DARK SAGE. The middle panel shows DARK SAGE results when the model seeds black holes like in TNG (i.e., if a halo of 5 × 1010 h −1 M ⊙ does not have a black hole of 106 M ⊙, then assign one). The right panel shows DARK SAGE galaxies when we apply our fixed conditional distribution, where we force galaxies to follow the black hole mass–halo mass median relation shown in TNG including the following black hole mass scatter values: 0, 0.2, and 0.4 dex. In this plot, we only display the black hole mass–halo mass median relation with a black hole mass scatter of 0.2 dex.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: The derived E vs. L  Z  distribution functions for the orbits of the stars in our combined primary + metal-poor annex sample, in six different bins of age (increasing upwards) and four different bins of metallicity (increasing to the right) for 24 total bins. We include 169,411 stars that satisfy our variability and blending criteria, for which the 1σ precision in the derived ages is better than 10%, and for which the 1σ precision in the derived [Fe/H] is better than 0.20 dex. Younger stars have nearly entirely disk-like kinematics, whereas older stars can be found in any region of kinematic phase space where there are stars to be found, including the disk.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: Left: the distribution in age–metallicity space for 242,489 stars from our primary sample which are not associated with open clusters, and which satisfy our other variability and blending inclusion criteria. Right: the distribution in age–metallicity space for 96,247 stars from our metal-poor annex which are not associated with open clusters, and which satisfy our other variability and blending inclusion criteria. The age–metallicity distribution functions show considerable structure that would not be discernible in either of the marginal distributions.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: Older stars can be found in any populated region of dynamic phase space, but younger stars are virtually purely associated with cold disk kinematics. The dynamical distribution of our sample stars in action space (left two panels) and in terms of integrals of motion (right panel). The points are color coded by their derived age, and the size of the points is proportional to their isolation in J  r −J  z  space.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: Color–magnitude diagrams of stars in M67 (left) and NGC 188 (right) color coded by the derived age, with the stars identified as variable or otherwise less reliable shown as cyan squares. Our analysis finds very little dispersion in the derived ages among the subgiant branch stars, but there is some contamination from stars that are likely to be blue stragglers.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: For stars in our metal-poor annex that have been observed by LAMOST. The cloud of stars for which the photometric metallicities are underestimated are largely a product of less reliable ultraviolet photometry and less certain reddening measurements. For the vast majority of stars, the astro-photometric metallicities are generally consistent with the spectroscopically derived metallicities
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: The scatter of the derived errors of the mean extinction coefficients as a function of the derived mean errors in the bolometric corrections, color coded by filter effective wavelength. The fact that the two variables are anticorrelated is indicative of undiagnosed systematic errors, such as errors in the assumed filter transmission curves.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: Comparison of our derived extinction values relative to those of the G. M. Green et al. (2019) maps (left) and the J. L. Vergely et al. (2022) maps (right). The black and white lines denote equality, and the blue line denotes the median trends. Both maps do well in the mean, but the predictions of G. M. Green et al. (2019) fare better for A  V  ⪆ 0.10, which comprise the majority of our primary sample.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: Distribution of the derived age precision for 335,778 stars in our combined primary sample and metal-poor annex that meet our quality inclusion criteria for variability and crossmatching between surveys. The median age precision is 9.5% and the mean age precision of 13.4%, with a long tail to higher errors.
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: An approximation of our selection function as a function of age and metallicity, where the selection weight is normalized to 1 for a star of solar age and metallicity. The selection function is close to uniform in the age–metallicity regime where stars are found in numerous numbers.
Paper: Could the Interband Lag of Active Galactic Nucleus Vary Randomly?
Authors: Zhen-Bo Su, Zhen-Yi Cai, Jun-Xian Wang, Tinggui Wang, Yongquan Xue, Min-Xuan Cai, Lulu Fan, Hengxiao Guo, Zhicheng He, Zizhao He, Xu-Fan Hu, Ji-an Jiang, Ning Jiang, Wen-Yong Kang, Lei Lei, Guilin Liu, Teng Liu, Zhengyan Liu, Zhenfeng Sheng, Mouyuan Sun, Wen Zhao
Figure caption: Left-hand panel: Distributions of the apparent r-band magnitudes for spectroscopically confirmed quasars in the SDSS DR16Q catalog (dotted histogram; B. W. Lyke et al. 2020) and a uniform, complete sample of broad-line AGNs at z < 0.35 selected from the SDSS DR7Q catalog (solid histogram; H.-Y. Liu et al. 2019). Note that only quasars with physical r-band magnitudes are used here. Shown for comparison are the spectroscopically complete limit of ∼19 mag for the SDSS quasars (vertical dotted line) and the WFST r-band 5σ detection limit of ∼23.7 mag in a single 90 s exposure (vertical dashed line; L. Lei et al. 2023), which is deeper than that of the SDSS-r band (vertical dotted–dashed line). Right-hand panel: The density map in ﹩\mathrm{log}{M}_{\mathrm{BH}}﹩ vs. ﹩\mathrm{log}{\lambda }_{\mathrm{Edd}}﹩ for local N5548-like AGNs expected in ∼1000 deg2, to be monitored by the WFST DHS, by scaling that of the H.-Y. Liu et al. (2019) sample covering 9376 deg2. The star and horizontal (or vertical) bar indicate the median and 16%–84% percentile ranges of ﹩\mathrm{log}{M}_{\mathrm{BH}}﹩ (or ﹩\mathrm{log}{\lambda }_{\mathrm{Edd}}﹩) of the H.-Y. Liu et al. (2019) sample.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Posterior probability distributions obtained with BEAGLE for our fiducial fits, along with the observed spectrum and model prediction, for JADES-GS-z11-0. From left to right, the columns show the stellar mass M *, star formation rate (SFR), age of the oldest stars t, (stellar and interstellar) metallicity Z, V-band attenuation optical depth ﹩{\hat{\tau }}_{V}﹩, ionization parameter ﹩{\rm{log}}\,{U}_{S}﹩, and UV slope β. The 1D (marginal) posterior distribution of each parameter is plotted along the diagonal, where the shaded gray regions represent the 1σ credible interval. The off-diagonal panels show the 2D (joint) posterior distributions, with the shaded blue regions representing the 1, 2, and 3σ credible intervals. In the top panel of the inset, we show the observed spectrum (red line), along with the model predictions (dark blue line). The model predictions at λ < 1450 Å are shown with a cyan line, to indicate that this region was masked during the fitting. In the bottom panel of the inset, we show the residuals in units of observed errors and the ±1σ region in gray.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: 2D and 1D NIRSpec PRISM/CLEAR spectra for JADES-GS-z11-0 (top) and JADES-GS-z13-0 (bottom), from the combined spectra from observations under PID 1210 as described in E. Curtis-Lake et al. (2023) and the new, deeper observations under PID 3215. In each panel, we plot the 2D spectrum underneath the sigma-clipped 1D spectrum. For the 1D spectrum, plotted in blue, we also plot uncertainties in light gray. We plot the positions of UV and optical emission lines with dashed lines at the fiducial redshifts estimated for each source. In an insert, we show the 2″ × 2″ JADES F444W+F200W+F090W RGB cutout with the MSA slitlets used for PID 3215 overplotted.
Paper: Could the Interband Lag of Active Galactic Nucleus Vary Randomly?
Authors: Zhen-Bo Su, Zhen-Yi Cai, Jun-Xian Wang, Tinggui Wang, Yongquan Xue, Min-Xuan Cai, Lulu Fan, Hengxiao Guo, Zhicheng He, Zizhao He, Xu-Fan Hu, Ji-an Jiang, Ning Jiang, Wen-Yong Kang, Lei Lei, Guilin Liu, Teng Liu, Zhengyan Liu, Zhenfeng Sheng, Mouyuan Sun, Wen Zhao
Figure caption: Top panels: Taking the median of 200 ideal lag-wavelength relations inferred from the mock WFST-ugriz LCs generated by the thermal fluctuation scenario, the median lag-wavelength relation steepens with increasing duration (﹩{ \mathcal M }﹩ from 3 months, through 6 and 9, to 12 months in one year; top left-hand panel) and baseline (﹩{ \mathcal Y }﹩ from 1 yr, through 2 and 6, to 10 yr with a fixed 6 months duration per year; top right-hand panel). Bottom panels: Same as the top panels, but for the prediction of the reprocessing model with DCE.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Same as in Figure 3, but for JADES-GS-z13-0 and also including the escape fraction f esc.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: NIRSpec PRISM/CLEAR spectroscopy (light blue lines) plotted against the ForcePho (red circles) and 0.″2 diameter circular aperture (black circles) NIRCam photometry for JADES-GS-z11-0 (left) and JADES-GS-z13-0 (right). In each panel, we compare to synthetic photometry measured from the NIRSpec PRISM data. The aperture photometry agrees well with the spectrum and synthetic photometry, while the ForcePho photometry is slightly larger than what is observed in the spectrum for JADES-GS-z11-0 and lower for JADES-GS-z13-0.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: The JADES-GS-z11-0 PRISM spectrum (blue) plotted against the NIRSpec G395M higher-resolution grating spectrum (red). Because of the difference in resolution between the two diffraction modes, we scale the y-axes differently for each spectrum, as shown on the left and right sides of the plot. At low significance, the [O II] and [Ne III] lines are visible in both spectra.
Paper: Could the Interband Lag of Active Galactic Nucleus Vary Randomly?
Authors: Zhen-Bo Su, Zhen-Yi Cai, Jun-Xian Wang, Tinggui Wang, Yongquan Xue, Min-Xuan Cai, Lulu Fan, Hengxiao Guo, Zhicheng He, Zizhao He, Xu-Fan Hu, Ji-an Jiang, Ning Jiang, Wen-Yong Kang, Lei Lei, Guilin Liu, Teng Liu, Zhengyan Liu, Zhenfeng Sheng, Mouyuan Sun, Wen Zhao
Figure caption: Same as Figure 7 but comparing the performance of different survey strategies of the ongoing and upcoming time domain surveys (see Table 1), adopting the same ﹩{ \mathcal Y }=1﹩ and ﹩{ \mathcal M }=6﹩.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: As in Figure 4, BEAGLE predictions and posterior probability distributions for JADES-GS-z13-0, but assuming a model with a delayed exponential SFH plus a 10 Myr burst, and no escape of ionizing photons.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Corner plot (left), SED fit (top), and SFH (middle) for JADES-GS-z11-0 from Prospector. In the corner plot, the first column from the left is galaxy redshift, the second column is stellar mass, the third column is the stellar metallicity, the fourth column is gas-phase metallicity, the fifth column is the ionization parameter of the gas, and the sixth column is the V-band optical depth for the older (>10 Myr) stellar population.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption:  ForcePho marginalized and joint posterior distribution for the half-light radius and semiminor to semimajor axis ratios b/a for JADES-GS-z11-0 (left) and JADES-GS-z13-0 (right).
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: As in Figure 4, BEAGLE predictions and posterior probability distributions for JADES-GS-z13-0, but assuming a model with constant SFH and no escape of ionizing photons.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Corner plot (left), SED fit (top), and SFH (middle) for JADES-GS-z13-0 from Prospector, with columns and description as in Figure 15.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: A schematic summarizing our methodology to identify high-probability WD+MS binary candidates in clusters, using the Pleiades as an example. (1) We define an initial Gaia DR3 stellar sample utilizing high-probability cluster members from T. Cantat-Gaudin et al. (2020). (2a) We preprocess and crossmatch the stellar sample with Pan-STARRS1 and 2MASS. (2b) We train an SVM classification model to identify stars that are photometrically similar to a known sample of WD+MS systems in SDSS. (3) We run the stellar sample from 2a through our SVM in 2b. The SVM computes the probability that each star in the sample is a WD+MS binary from high-dimensional input photometry. (4) For each candidate identified with P > 0.9, we first vet its SED and then examine the spatial locations and kinematics relative to a sample of known cluster members. (5) High-probability candidate WD+MS binaries are identified. (6*) We perform follow-up spectroscopy and/or analyze existing light-curve data for an example subset of high-probability systems.