adsabs/AstroCLIMB huggingface dataset:
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: Model magnitude–color sequences for a WD of T eff = 15 kK to 200 kK with radii of R = 0.03 and 0.02 R ⊙ at the distance of the target. A pair of identical WDs would be shifted upward correspondingly to twice the flux, i.e., by 0.75 mag. The target’s measured GALEX NUV magnitudes are shown with horizontal dashed lines (gray shadowed areas show the uncertainties), and the NUV − UVM2 color with a vertical line. Model magnitudes are reddened with two different extinction types (R  V  = 3.1, black; R  V  = 2, purple sequences) and different amounts of extinction, for illustration purposes. The plot shows that (i) a WD or WD pair (or a cooler main-sequence star, not shown) could account for the GALEX and Swift NUV measurements, unexplained by a red giant SED (ii) from NUV-only data, T eff is degenerate with radius and E  B−V ; therefore, FUV imaging and a UV−optical spectrum were obtained to test the presence of a hot companion and to constrain its parameters if present.
Paper: Disk2Planet: A Robust and Automated Machine Learning Tool for Parameter Inference in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Kwang Moo Yi, Lu Lu, Sifan Wang, Paris Perdikaris
Figure caption: Representative examples of the input data sets, and the corresponding parameter inference uncertainties (σ). The input data sets contain images of, from top to bottom, Σ (a), Σ + v LOS (b), Σ + v  r  + v  θ  (c), Σ with noise (d), Σ + v LOS with noise (e), radially cropped Σ (f), and azimuthally cropped Σ (g). 256 tests are run for each. The uncertainties are calculated as half the difference between the error distribution’s 84th and 16th percentiles. The numbers on the bar plot represent the uncertainties for the baseline data set (a), and how the uncertainties in the other data sets (b)–(g) compared to those in the baseline case.
Paper: Disk2Planet: A Robust and Automated Machine Learning Tool for Parameter Inference in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Kwang Moo Yi, Lu Lu, Sifan Wang, Paris Perdikaris
Figure caption: Corner plots showing the distribution of errors in the inferred parameters (Equation (4)). Corresponding panels on the two sides are on the same scales. The histograms on the diagonal show the distributions of individual parameters, while the off-diagonal panels highlight pairwise correlations. See Section 3.1 for details.
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: The shortest wavelength portion of the STIS spectrum, here with flux (erg cm−2 s−1 Å−1) plotted in linear scale to better distinguish significant flux from noise level, and to illustrate the sensitivity of this range to the companion, whose flux becomes stronger than the RG’s flux. Without this spectral region, the rest of the spectrum could be fit by a wider combination of T eff and E  B−V  values for the stellar pair. Models with metallicity Z = 0.002 are used in the top panel, and Z = 0.006 in the bottom panel, as in Figures 2 and 3, respectively. The different metallicity hardly affects the RG continuum flux over a wide optical-IR range, as shown in the two previous figures, but the difference becomes significant in this range, where the fit to the composite spectrum is compensated by the companion’s solution, requiring a radius of 4.2 R ⊙ in the lower plot vs. 2.7 R ⊙ in the upper plot, and a slightly cooler T eff.
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: Mg II doublet emission in the STIS G230L spectrum of 2MASS J05215658+4359220 (thick line) compared with two IUE spectra of UZ Lib, a chromospherically active RG (thin solid and dashed lines). The fluxes of each IUE spectrum (LWP5711 and LWP5764) have been scaled to match the local continuum level of our target around the Mg II line. A caveat must be considered in the comparison: in 2MASS J05215658+4359220 the companion significantly contributes to the flux at these wavelengths (Figures 2 and 3 bottom panel, and Figure 4); subtracting its contribution (cyan models in Figure 4) would make the Mg II emission much stronger. A simple scaling by radius and distance is not possible because differential reddening should also be accounted for, which is uncertain for UZ Lib. Although sampled with a ∼2.66 Å step, the IUE spectra have an actual resolution of ∼6 Å, lower than the STIS G230L spectra. The STIS resolution has not been degraded in the plot.
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: WFC3 images of the source in the five filters arranged from shorter to longer effective wavelength; repeated in different rows using increasing contrast. Images are 50 × 50 pixel cutouts (one pixel is 0.″04). For the dithered exposures, the pictures were produced from the drizzled images, therefore the resolution is slightly degraded with respect to the full resolution of individual exposures.
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: The STIS G230L combined data sets oemq01010+oemq01050 (dotted line) are consistent with an upper limit of 10−17 erg cm−2 s−1 Å−1 shortwards of ∼2300 Å. The squares are averages in 100 Å bins.
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: HR diagram of PARSEC evolutionary tracks for metallicity Z = 0.006; the main-sequence phase is shown in green. The red star marks the RG position, and the cyan diamond is the companion. The bottom panels zoom around the locus of each star: in the left panel (RG) tracks with masses of 0.9, 1.1, 1.3, 1.5, and 1.7M ⊙ (from the bottom right toward the top left) are marked with thick black lines, and tracks for masses of 1.0 and 1.05M ⊙ are shown in orange; in the right-bottom panel, thick-line tracks have masses of 1.3, 1.5, and 1.7M ⊙.
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: HR diagram of PARSEC evolutionary tracks for metallicity Z = 0.002; the main-sequence phase is shown in green. The red star marks the RG position and the cyan diamond the companion, using the parameters derived with models of metallicity Z = 0.002 (Figure 2). In the left panel, the loops of the evolutionary tracks do not reach the T eff derived for the RG; in the right panel, thick-line tracks have masses of 1.0, 1.3, and 1.5M ⊙.
Paper: A Promising Approach for Determining Neutrino Mass Hierarchy by Using Supernova Neutrino Detections
Authors: Gexing Li, Zhihong Li
Figure caption: If a CCSN explodes at a distance of 10 kpc and the emitted neutrinos are detected by an ideal detector with a water mass of 1 kt, the color contours represent the expected event rates of the ﹩{\bar{\nu }}_{e}﹩ in the energy range 10 ∼ 20 MeV, varying with the postbounce time and the neutrino energy. The title of each panel shows the PNS baryon mass and the neutrino mass-hierarchy model. Δ(NH−IH) represents the difference of the event rates obtained by using the NH and IH models. The high-density nuclear EOS is taken as DD2.
Paper: A Promising Approach for Determining Neutrino Mass Hierarchy by Using Supernova Neutrino Detections
Authors: Gexing Li, Zhihong Li
Figure caption: If a CCSN explodes at a distance of 10 kpc and the emitted neutrinos are detected by an ideal detector with a water mass of 1 kt, the expected cumulative event numbers vary with the numbers of the ﹩{\bar{\nu }}_{e}﹩, with energies 10 ∼ 20 MeV arriving at the Earth within the postbounce time 0 ∼ 10 s for different PNS baryon masses, EOSs, and neutrino mass hierarchies.
Paper: A Promising Approach for Determining Neutrino Mass Hierarchy by Using Supernova Neutrino Detections
Authors: Gexing Li, Zhihong Li
Figure caption: For a CCSN exploding at a distance of 1 kpc, the expected cumulative event numbers of the ﹩{\bar{\nu }}_{e}﹩ on an ideal detector with water mass of 1 kt at the postbounce times 0.5 and 1.0 s are shown, varying with the PNS baryon mass and the ﹩{\bar{\nu }}_{e}﹩ survival probability. The red dashed and white dotted lines represent the ﹩{\bar{\nu }}_{e}﹩ survival probability predicted by the adiabatical MSW conversion models.
Paper: A Promising Approach for Determining Neutrino Mass Hierarchy by Using Supernova Neutrino Detections
Authors: Gexing Li, Zhihong Li
Figure caption: The minimum required water mass of neutrino detectors to distinguish NH from IH for CCSNe at different distances and with different PNS baryon masses. The upper and lower panels show the results by using the neutrino events within the postbounce times 0.5 and 1.0 s, respectively.
Paper: A Promising Approach for Determining Neutrino Mass Hierarchy by Using Supernova Neutrino Detections
Authors: Gexing Li, Zhihong Li
Figure caption: The cumulative numbers of ﹩{\bar{\nu }}_{e}﹩ and ﹩{\bar{\nu }}_{x}﹩ with energies 10 ∼ 20 MeV before the MSW effects in the postbounce time 0 ∼ 1 s for different PNS baryon masses.
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: Raw (upper) and phase-folded (bottom) radial velocity curves of the binary system (blue) and the third star (orange). The dots represent our measurements. The blue squares are values determined by J. A. Eaton & G. W. Henry (2007) and the orange squares represent the values derived by L. V. Glazunova et al. (2008).
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: The black lines represent the LSD profiles of SZ Psc at two different phases, while the orange lines show the initial fits. The blue and red lines above each LSD profile indicate the residual and the corresponding Gaussian fit, respectively.
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: Cross-correlation functions of each latitude band for the K star of SZ Psc. The peak (white open circle) of the CCF for each latitude is derived by fitting a Gaussian profile, and the FWHM of the profile is plotted as the white horizontal line. The orange curve is the fit of the solar-like differential rotation law.
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: Tests on the effect of the phase coverage with the simulated images. The first panel is the input image used to produce the profiles. The others are reconstructed images from the simulated data sets with different phase sampling.
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: Surface reconstructions of the K component of SZ Psc for 2014–2018. The observed phases are marked as the vertical ticks at the bottom of each image.
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: The maximum-entropy-regularized fits to the observed LSD profiles of SZ Psc for the 2014, 2015, and 2016 data sets.
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: Same as Figure 6, but for the 2017–2018 data sets.
Paper: Further Study of Starspot Activity and Measurement of Differential Rotation for SZ Piscium
Authors: Yue Xiang, Shenghong Gu, A. Collier Cameron, J. R. Barnes, Dongtao Cao
Figure caption: Same as Figure 6, but for the 2017 data sets.
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption: Probability distributions of q, T 2, i, f, L 1g /L  Tg , ﹩{L}_{1r}/{L}_{{Tr}}﹩ , L 1i /L  Ti , L 3g /L  Tg , ﹩{L}_{3r}/{L}_{{Tr}}﹩, and L 3i /L  Ti  determined by the MCMC modeling of J005148.
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption: Probability distributions of q, T 2, i, f, L 1g /L  Tg , ﹩{L}_{1r}/{L}_{{Tr}}﹩, L 1i /L  Ti , T  s , r  s , and λ determined by the MCMC modeling of NSVS 503993.
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption: The relationship between log M  T  and log J orb. The crosses represent detached binaries, the solid circles display contact binaries, and the open circles denote our eight targets. The dashed line refers to the boundary between detached and contact binaries derived by Z. Eker et al. (2006).
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption: Probability distributions of q, T 2, i, f, L 1g /L  Tg , ﹩{L}_{1r}/{L}_{{Tr}}﹩, and L 1i /L  Ti  determined by the MCMC modeling of J005148.
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption:  O − C diagrams for our eight targets.
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption: The fitting results for each target. The scatter points are the real observed data, the curves are the fitting results, and the fitting residuals are shown in the lower panel. The data set used to create these light curves is available for download.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption:  M–L and  M–R diagrams. The solid line is the ZAMS and the dotted line is the TAMS. The circles represent the primary components and the triangles represent the secondary components.
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption: The fitting results of each target after incorporating l 3. The scatter points are the real observed data, the curves are the fitting results, and the fitting residuals are shown in the lower panel.
Paper: Photometric and Spectroscopic Analysis of Eight Totally Eclipsing Contact Binaries with Small Mass Ratios
Authors: Li-Heng Wang, Kai Li, Ya-Ni Guo, Jing-Yi Wang, Xiang Gao, Xing Gao, Guo-You Sun
Figure caption: Using ULySS to fit the spectral data. The black line represents the original data and the red line represents the fitted data.
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Kepler’s demographic cliff, visible in the rotation-derived age distributions of its stars (left) and planet hosts (middle). The top row shows stars with temperatures of 3800–6200 K. Opaque lines impose quality cuts on binarity, metallicity, crowding, and the star’s evolutionary state; transparent lines do not (see Section 4.1). The bottom row shows stars with temperatures of 4400–5400 K, which have more precise ages. The statistical uncertainty for an average star at 1, 2, and 3 Gyr is shown, and is identical across each row. Finally, the right panel compares the rotational ages against SFHs derived from color–magnitude diagram (CMD) fits to other regions of the Galaxy (dashed and dotted lines). Completeness in Kepler’s P rot detection sensitivity is near unity until t ≲ 3 Gyr, and decreases rapidly at older ages (K. Masuda 2022a).
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Reported ages of individual stars in benchmark open clusters. Each point denotes a star’s reported age, normalized by the age of a stellar ensemble in which the star is a candidate member. Cluster membership was evaluated without knowledge of rotation, and for this plot, no attempt was made to exclude known binaries. Although some field interlopers may be present in the membership lists, outliers can be compared between different methods on a relative basis. Each study was cross-matched against the same cluster list; certain methods report ages for more stars than others. Horizontal scatter is added to visually clarify the statistical age uncertainties. Below 1 Gyr, our ages are generally accurate, and their statistical uncertainties match their dispersion.
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: The stars: our analysis focuses on stars observed by Kepler with previously reported rotation periods (gray points). The rotation periods are primarily drawn from A. R. G. Santos et al. (2019, 2021). About half of the stars with rotation periods are suitable for gyrochronology (dark gray), based on factors including their apparent nonbinarity and proximity to the main sequence (orange line in upper panel; see Section 4.1). Some host “confirmed” or “candidate” KOIs that meet additional planetary quality criteria (yellow points; Section 4.2). Surface gravities and effective temperatures were derived photometrically by T. A. Berger et al. (2020b). Isochrones in the upper panel are from MIST (J. Choi et al. 2016).
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Rotation periods for Kepler target stars (left) and known planet hosts (right). The gray lines are polynomials fitted to the slow rotation sequences of open clusters. The 2D histogram of the stellar sample (left) shows only apparently single stars near the main sequence with ﹩\mathrm{log}g\,\gt ﹩ 4.2, renormalized unit weight error (RUWE) < 1.4, and temperatures of 3800–6200 K. The planet hosts (right) require the same stellar cuts, and include only the confirmed and candidate planets described in Section 4.2. The total number of stars N s and planets N p are noted in the relevant panels. A simple estimate for the number of young planets discovered by Kepler follows by counting points below the rotational isochrones.
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: The models: points represent 104 draws from models that have been fitted to rotation periods (L. G. Bouma et al. 2023) and lithium equivalent widths (EWs; R. D. Jeffries et al. 2023) of stars in open clusters. Lines are the “mean models” at various ages. The intrinsic dispersion around the mean, which is what the models fit, sets the theoretical precision floor for the age-dating methods. Additional sources of uncertainty, including measurement uncertainty, impose further limits. These models are calibrated using data from open clusters. The sizes of the points are the same in each panel, so that low apparent density signifies greater dispersion around the mean.
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Equivalent widths (EWs) of the Li I 6708 Å doublet for planet-hosting stars. These measurements were made from Keck/HIRES spectra collected from 2009 to 2024. Lines are the “mean” isochrones from R. D. Jeffries et al. (2023). The intrinsic dispersion around these isochrones becomes much larger than changes in the mean at ≳1 Gyr (see Figure 4). Some stars with lithium detections do not have detected rotation periods, and vice versa.
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Sizes, orbital periods, and rotation-based ages of transiting exoplanets younger than 1 Gyr. Systems are selected to have t <1 Gyr at 2σ. Star symbols denote 46 planets characterized in this work to have such ages at the highest confidence, meaning that none of Q star bits 0–10 are raised, and the planets have no quality flags raised. Transparent crosses denote 17 planets for which either the planet is grazing, or the star has RUWE > 1.4. Gray points are from the NASA Exoplanet Archive.
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Potential impact of unresolved binaries. This figure shows the same raw (thinnest line) and quality-flag cleaned (“gyro applicable”) distributions as in Figure 6. However, even after applying our quality cuts, up to 1190 of 2706 apparently clean rotators with P rot < 10 days could be unresolved ≲0.5 au binaries (see Section 8.2). The dark blue “5% binary contamination” distribution corrects for this possibility by randomly removing what we estimate (estm.) to be the maximum possible number of such systems; the true correction might be smaller. We expect such a correction to be more important in the sample of all Kepler stars than in the KOI host sample.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: VULCAN PHO network results of VMRs (colored solid lines) for comparison to the D. Wang et al. (2017; their Figure 2) results. The chemical equilibrium volume mixing ratios are denoted by the colored dashed lines. This shows results for various PHO species of interest across the hot Jupiter T–p profiles with equilibrium temperatures T eq = 500, 1000, 1500, and 2000 K (black dotted lines; D. Wang et al. 2017). A constant K zz = 109 cm2 s−1 and solar metallicity is assumed as in D. Wang et al. (2017).