adsabs/AstroCLIMB huggingface dataset:
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: The top panel shows the distribution of the derived planetary radii as a function of orbital periods along with the associated KDE. The middle and bottom panels show the same KDE, along with our radius gap relation (black solid line), and uncertainties (gray region). Middle panel: the radius gap relation from R. Cloutier & K. Menou (2020) for KM dwarfs is depicted as a maroon dashed line, the relation from C. F. Martinez et al. (2019) for FGK dwarfs and V. Van Eylen et al. (2018) for M dwarfs are depicted as a green dashed line, and the relation from E. Gaidos et al. (2024) for M dwarfs is depicted as a blue dashed line. Bottom panel: prescriptions from different models. Red, purple, cyan, gray, and orange-dashed lines represent, respectively, models for gas-poor formation (E. D. Lopez & K. Rice 2018), photoevaporation (E. D. Lopez & K. Rice 2018), core-powered mass loss (A. Gupta & H. E. Schlichting 2019), impact erosion (M. C. Wyatt et al. 2020), and pebble accretion (J. Venturini et al. 2024).
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: Left panel: density histogram of our exoplanetary sample with available masses from the literature. The dashed lines indicate the boundaries for segregating exoplanets into three groups. Middle panel: derived planetary radii as a function of planetary mass, along with mass–radius relations from L. Zeng et al. (2019) associated with “rocky” (black line), “50% Fe” (gold line), and “50% H2O” (cyan line) compositions. We also show gray and red-dashed lines representing rocky compositions with 0.1% H2 atmospheres, for equilibrium temperatures of respectively 300 K and 700 K. Exoplanets that fall between densities between 0.5 and 0.9 ρ⊕ are depicted in cyan. The Earth’s position is also shown for comparison. Right panel: the exoplanetary mass–density diagram.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: Left panel: exoplanetary radii as a function of orbital periods, where sample exoplanets, having masses available, which fall on the “rocky” side of the gap are colored in gold, while those falling on the sub-Neptune side of the gap are colored in blue. Gray xs are exoplanets in our sample without available mass measurements. Right panel: exoplanetary densities as a function of orbital period following the same color scheme, for exoplanets with ρp < 1.6 ρ⊕. Typical uncertainty in the density is shown in the left bottom of the figure.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: Top panel: stellar radii as a function of M﹩{}_{{{\rm{K}}}_{{\rm{s}}}}﹩ for our APOGEE sample are shown as blue circles. The second-degree polynomial fit for our data is represented as a black line, and is given by R* = 1.7420 −0.2925 M﹩{}_{{{\rm{K}}}_{{\rm{s}}}}﹩ + 0.0123 M﹩{}_{{{\rm{K}}}_{{\rm{s}}}}^{2}﹩. The gray region shows the derived uncertainties in stellar radii as a function of M﹩{}_{{{\rm{K}}}_{{\rm{s}}}}﹩. The bottom panel shows the residuals between our derived radii and the calibration.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: Distribution of the derived planetary radii for our full sample is shown in blue. The gray-dashed line indicates the minimum probability density at 1.78 R⊕ for a KDE associated with the full sample. The histogram of the planetary radii distribution, obtained from the spectroscopic analysis of the APOGEE sample, is delineated in white.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: Distribution of the derived planetary radii as a function of insolation, along with the associated KDE.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: Comparison between the planetary radii from this work with results from the literature. Blue, orange, and gray circles are radii obtained from the ExoFOP TOI Program, KOI DR25 (S. E. Thompson et al. 2018), and other works from the literature. The x = y relation is shown by the gray-dashed line.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: From left to right: distribution of Gaia distances from C. A. L. Bailer-Jones et al. (2021), M﹩{}_{{{\rm{K}}}_{{\rm{s}}}}﹩ absolute magnitudes, and stellar radii for the 161 M dwarfs in our full sample. As a comparison we also show the histograms for the APOGEE sample delineated in white.
Paper: Chandra/HETG and NuSTAR Observations of V750 Ara, a γ Cas-type Star
Authors: David P. Huenemoerder, Sean J. Gunderson, Richard Ignace, Joy S. Nichols, A. M. T. Pollock, Pragati Pradhan, Norbert S. Schulz, Dustin K. Swarm, José M. Torrejón
Figure caption: HETG spectrum of V750 Ara in black, which is the merged HEG and MEG first orders, the HETG zeroth order in cyan, and the NuSTAR spectrum in blue (combined FPMA and FPMB). In red is a model using an absorbed cooling-flow model plus a Gaussian for a tentative Fe K fluorescence line. Features with significant detections are marked below the spectrum. The bottom panel shows the residuals in the form of the delta-Cash statistic (ΔC), appropriate for Poisson distributed counts, normalized by its square-root absolute value (﹩| {\rm{\Delta }}C{| }^{\frac{1}{2}}﹩), to make it analogous to the commonly used normalized Δχ statistic. Colors are as in the upper panel.
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: Merger rates vs. redshift for various subpopulations of MBHBs. The left panel shows the total merger rate (gray line) as well as the merger rate for the subpopulations of isolated binaries (orange), weak triple systems (light blue), and strong triples (dark blue). The middle panel shows the merger rate for strong triples, divided into those resulting from the prompt merger scenario vs. the merger after kick scenario. In the right panel, the merger rate for the stalled model (red dashed line) is shown in comparison to the fiducial merger rate (gray). The cumulative merger rates observed at z = 0 for isolated binaries, weak triples, and strong triples are 0.37 yr−1, 0.017 yr−1, and 0.023 yr−1, respectively. The merger rate in the stalled model is suppressed by a factor of ∼5 compared to the fiducial model.
Paper: Chandra/HETG and NuSTAR Observations of V750 Ara, a γ Cas-type Star
Authors: David P. Huenemoerder, Sean J. Gunderson, Richard Ignace, Joy S. Nichols, A. M. T. Pollock, Pragati Pradhan, Norbert S. Schulz, Dustin K. Swarm, José M. Torrejón
Figure caption: NuSTAR light curve (top left) in 200 (gray) and 5828 s bins (red). The larger bin size was chosen to match the period of the NuSTAR orbit. On the top right we show the PSD of the light curve, which shows a slope indicative of red noise, flickering at amplitudes larger than expected from Poisson noise. We did not have enough sensitivity to reach the Poisson noise floor. Blue tick marks at the top indicate the NuSTAR orbital frequency and harmonics, none of which are evident in the transform. Bottom: the HETG light curve of dispersed events in 1 ks bins, with the observations concatenated in time order in alternating colors. The NuSTAR observation is between the two observations at about 95 ks. Count rates are given in s−1. The PSD is a unitless normalized probability.
Paper: Chandra/HETG and NuSTAR Observations of V750 Ara, a γ Cas-type Star
Authors: David P. Huenemoerder, Sean J. Gunderson, Richard Ignace, Joy S. Nichols, A. M. T. Pollock, Pragati Pradhan, Norbert S. Schulz, Dustin K. Swarm, José M. Torrejón
Figure caption: Line widths and offsets from Gaussian fits. Only features that provided meaningful constraints are shown. Confidence limits are 1σ. H-like feature velocities are in reference to the emissivity-weighted mean of the doublet’s wavelengths. The Mg XI He-like resonance, intercombination, and forbidden lines had their relative positions constrained and a common width parameter. Widths are the intrinsic value required in addition to instrumental broadening.
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: Distributions of the merging BH mass ratio (qmrg), total mass (Mmrg), and redshift (z) of the merging MBHs in the subpopulations of isolated binaries, weak triples, and strong triples. The median mass ratio of mergers in strong triples, weak triples, and isolated binaries is 0.63, 0.40, and 0.25, respectively. 64% of strong triple mergers have qmrg > 0.1. The median total mass of mergers in strong triples, weak triples, and isolated binaries is 7.87 × 107 M⊙, 9.72 × 107 M⊙, and 3.89 × 107 M⊙, respectively.
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: A 2D histogram in the ﹩{\rm{log}}{q}_{\rm{in}}\rm{--}{\rm{log}}{q}_{\rm{out}}﹩ plane for prompt mergers (left panel) and merger after a slingshot kick (right panel) from triple interactions. The red dots correspond to triple-induced mergers where the inner binary would not have merged in isolation, and they are plotted for all realizations of the strong triple outcomes. The distribution highlights that the prompt mergers are predominantly seen in equal-mass triples. Additionally, prompt mergers involve a higher fraction of cases where the binaries would have otherwise stalled in isolation compared to mergers after kick.
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: Normalized distributions of the three models for premerger MBH spins considered in this work: random (solid dark blue), cold (dashed light blue), and aligned (solid red). Top panel: distribution of misalignment angle of the spins. Bottom panel: distribution of spin magnitude of the models.
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: Schematic diagram illustrating the outcomes of binary and triple interactions in the subpopulation of Illustris MBH binaries that form strong triples. Triple interactions are added for the strong triple subpopulation (atriple < 100 pc). Merger fractions averaged over 100 realizations are indicated for the three outcomes: (i) prompt merger (21%), (ii) merger after kick (48%), and (iii) no-merger (31%).
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: The velocity distributions are shown for GW recoil and slingshot kicks to MBHs in our model. GW recoil velocities are shown for each spin model (random, aligned, and hybrid) and are averaged over all realizations of premerger MBH spins. The mean recoil velocity is plotted with a shaded region indicating the 1σ spread. Slingshot kick velocities are averaged over all realizations of strong triple interaction outcomes. GW recoil from random spins produces the highest median kick velocity (314 km s−1), followed by slingshot kicks (283 km s−1). 16% of GW recoil kicks are above 1000 km s−1 in the random spin model, compared with 10% of slingshot kicks.
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: Ejection rates vs. redshift from GW recoil kicks are shown for each spin model: random (red dotted), hybrid (light blue, dotted–dashed) and aligned (dark blue, dashed) spins. Also shown is the ejection rate from slingshot kicks (solid green), compared with the total merger rate (black dashed). The left panel shows the ejection and merger rates for the total MBHB population, while the right panel shows only the subpopulation of strong triples. The ejection rates are averaged over all realizations. GW recoils from random spins dominate the ejections in the total population, contributing to ∼7% of the total MBH population being ejected. Within strong triples, slingshot kicks become significant with ∼7% of them resulting in an ejection.
Paper: Mergers and Recoil in Triple Massive Black Hole Systems from Illustris
Authors: Pranav Satheesh, Laura Blecha, Luke Zoltan Kelley
Figure caption: The number of mergers vs. redshift is shown for subpopulations of the Illustris MBH merger population. The green dotted line shows the total number of mergers, while the orange dotted line shows the mergers in strong triples. The solid green line show the subset of these mergers that are both massive (Mmrg > 108 M⊙) and major (qmrg > 0.1). The solid orange line shows mergers in strong triples for the massive major merger subset. Strong triple mergers contribute to 19% of the massive major merger population.
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Contour plots in the y = 0, xz−plane displaying the time evolution of the jy, ﹩\rho ^{\prime} ﹩, ﹩p^{\prime} ﹩, and ﹩e^{\prime} ﹩ for the baseline case, ψ = 0.05, between t = 0.1–6.5. The magenta lines represent the equipartition layer, and the black magnetic field lines indicate the magnetic skeleton where the z-axis is the spine and the x-axis corresponds to the relevant field lines that make up the fan plane. Note that the saturation scale varies between subfigures to show the detail.
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Contour plots in the y = 0, xz−plane displaying the time evolution of the ﹩p^{\prime} =p-\overline{p}﹩ contours for simulations ψ = 0.01, ψ = 0.025, ψ = 0.05, and ψ = 0.1 (corresponding to the first, second, third, and fourth columns, respectively). Note that the third column of Figure 5 is identical to that of the third column of Figure 2, but is replicated here to ease comparison. The magenta lines represent the equipartition layer, and the black magnetic field lines indicate the magnetic skeleton, where the z-axis is the spine and the x-axis corresponds to the fan plane. Note that the saturation scale varies between subfigures to show the detail.
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Traced magnetic field lines for the initial condition, Equations (6)–(8). The green line represents the spine of the null point, while the blue and red lines represent the fan plane traced from the upper and lower boundaries, respectively. Panels (d)–(f) represent the initial condition for the baseline case, which extends J. Thurgood et al. (2017). Panels (a)–(c) present the initial condition for our smallest perturbation amplitude (ψ = 0.01) and panels (g)–(i) for the largest perturbation amplitude considered (ψ = 0.1).
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Contour plots or ﹩\rho /\overline{\rho }﹩, ﹩p/\overline{p}﹩, and ﹩e/\overline{e}﹩ normalized by their initial state for the ψ = 0.05 case at t = 60. The magenta lines represent the equipartition layer. The top row shows the y = 0, xz−plane, where the black magnetic field lines indicate the magnetic skeleton, where the z-axis is the spine, and the x-axis corresponds to the fan plane. The bottom row shows the z = 0, xy−plane.
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: The evolution of jy(0, 0, 0, t), measured at the null point and normalized by the initial perturbation amplitude, ψ, for ψ = 0.01, 0.025, 0.05, and 0.1. Insets show the same evolution but over subsets of time (to show further detail).
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Contour plots in the y = 0, xz−plane displaying the time evolution of the jy, ρ, ﹩p^{\prime} ﹩, and ﹩e^{\prime} ﹩ for the baseline case, ψ = 0.05, for later time steps. The magenta and black lines have the same meaning as in Figure 2.
Paper: Chemical Abundances of M and G Dwarfs in the Hyades and Coma Berenices Open Clusters from APOGEE Spectra
Authors: Deusalete Vilar, Diogo Souto, Katia Cunha, Anderson Andrade-Silva, Verónica Loaiza-Tacuri, Fábio Wanderley, Verne V. Smith, Vinicius Grilo, Cintia F. Martinez, Bárbara Rojas-Ayala, Zachary Way
Figure caption: Left panel: a CMD diagram showing (J–Ks) vs. J for our sample of selected stars, with the red circles representing the Hyades and the blue triangles Coma Berenices. Open symbols represent M, and filled symbols represent the G dwarf stars. Four MIST isochrones of different ages are shown: 650 (solid line) and 700 Myr (dashed). Right panel: a Kiel diagram for the Hyades and Coma Berenices. Symbols are the same as those in the left panel, but with values from the OCCAM (N. Myers et al. 2022) survey as gray inverted triangles.
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: (a) Isosurfaces of Q criterion showing vortex rolls colored by ωz, where the black line represents the spine. (b) shows a time–distance diagram of the circulation, Γ(z, t), integrated over the xy-plane at every position along the z-axis for the ψ = 0.05 case. Red crosses indicate the roots of jy(0, 0, 0, t) and the black line represents the averaged equipartition layer. Dashed lines correspond to z = 0.5, 1, and 1.5. (c) plots the Γ(z, t) at three different heights, z = 0.5, 1, and 1.5, taken from the dashed lines in (b).
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Period extraction for the baseline case. (a) Current density at the null point, jy(0, 0, 0, t). (b) jy(0, 0, 0, t) wavelet power spectrum, where the white-hatched region represents the cone of influence. (c) Dominant period obtained from the wavelet power map at each time step by applying a Gaussian fitting, where the blue line shows the Gaussian mean and the shaded area the estimated error using the Gaussian standard deviation. The dashed line shows the average period obtained from t = 0 to 60.
Paper: Chemical Abundances of M and G Dwarfs in the Hyades and Coma Berenices Open Clusters from APOGEE Spectra
Authors: Deusalete Vilar, Diogo Souto, Katia Cunha, Anderson Andrade-Silva, Verónica Loaiza-Tacuri, Fábio Wanderley, Verne V. Smith, Vinicius Grilo, Cintia F. Martinez, Bárbara Rojas-Ayala, Zachary Way
Figure caption: Elemental abundance distributions for the Hyades (top panel) and Coma Berenices (bottom panel) open clusters, presented as violin diagrams. Each violin shows the distribution of abundances derived for all studied elements, combining both G and M dwarf stars. The black dashed line indicates the overall mean metallicity ([M/H]) considering all studied elements for each cluster.
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Current density jy(0, 0, 0, t) measured at the null point compared with the best-fit functions g2 and f1 from Equations (17) and (20), respectively.
Paper: Chemical Abundances of M and G Dwarfs in the Hyades and Coma Berenices Open Clusters from APOGEE Spectra
Authors: Deusalete Vilar, Diogo Souto, Katia Cunha, Anderson Andrade-Silva, Verónica Loaiza-Tacuri, Fábio Wanderley, Verne V. Smith, Vinicius Grilo, Cintia F. Martinez, Bárbara Rojas-Ayala, Zachary Way
Figure caption: Chemical abundance comparison between M and G dwarf stars in the studied open clusters Hyades and Coma Berenices. The red circles represent the mean abundances for the Hyades and the blue triangles for Coma Berenices. The δ abundance value (G dwarfs–M dwarfs) is indicated in the top-left corner of each panel.
Paper: Chemical Abundances of M and G Dwarfs in the Hyades and Coma Berenices Open Clusters from APOGEE Spectra
Authors: Deusalete Vilar, Diogo Souto, Katia Cunha, Anderson Andrade-Silva, Verónica Loaiza-Tacuri, Fábio Wanderley, Verne V. Smith, Vinicius Grilo, Cintia F. Martinez, Bárbara Rojas-Ayala, Zachary Way
Figure caption: Comparison of chemical abundances between stars in the studied open cluster Hyades (gray) and the works of R. Carrera & E. Pancino (2011; brown) and L. Casamiquela et al. (2020; yellow).
Paper: The Periodicity of Three-dimensional Oscillatory Reconnection
Authors: Luiz A. C. A. Schiavo, Gert J. J. Botha, James A. McLaughlin
Figure caption: Fourier spectra for jy(0, 0, 0, t)/ψ, for initial perturbation amplitudes ψ = 0.01, 0.025, 0.05 and 0.1.
Paper: Chemical Abundances of M and G Dwarfs in the Hyades and Coma Berenices Open Clusters from APOGEE Spectra
Authors: Deusalete Vilar, Diogo Souto, Katia Cunha, Anderson Andrade-Silva, Verónica Loaiza-Tacuri, Fábio Wanderley, Verne V. Smith, Vinicius Grilo, Cintia F. Martinez, Bárbara Rojas-Ayala, Zachary Way
Figure caption: Chemical abundance distribution ([X/Fe] vs. [Fe/H]) of G and M dwarfs in the open clusters studied in this work, compared to values from the OCCAM DR17 (N. Myers et al. 2022). The red circle represents the Hyades, the blue triangles are from Coma Berenices, and the gray inverted triangles are results from the OCCAM star.