adsabs/AstroCLIMB huggingface dataset:
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Histogram of mean ρ in bins of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩1, computed over all epochs and all filters, for all the resolutions presented in Table 2. The inlet shows the histogram for objects with ρ smaller than 100 mas in bins of 10 mas.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Histogram of mean Δm in bins of 0.5 mag, computed over all epochs for the blue filter (left) and the red filter (right), for all the resolutions presented in Table 2.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Calibration of Zorro astrometry relative to SOAR. The top panel shows the scale ratio, while the bottom panel shows the difference in θ for the calibration binaries included in the 2019A run. The solid line shows the mean, while the dashed lines indicate the  ±1σ range.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Same as the fourth row in Figure 9, except that the top row is for the range with ﹩\rho \lt 0\mathop{.}\limits^{^{\prime\prime} }4﹩ (program stars), while the bottom row is for the larger ρ binaries (mostly astrometric standards).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: TESS light-curve analysis for TOI-4364b. Top: unflattened, processed light curve of TOI-4364. Middle: flattened, systematically corrected light curve (gray) with the best-fit batman (green). Bottom: phase-folded light curve with binned points (purple) and the phase-folded best-fit transit model (green).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: TSM (top panel) and ESM (bottom panel) values as a function of planet radius for TOI-4364b (star), the population of confirmed exoplanets (gray circles), and young planets with well-constrained ages (<1 Gyr; larger circles). The blue shaded region indicates the location of the radius valley as in B. J. Fulton et al. (2017).
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: (a) Interpolated age and mass distributions from CBPD23 evolutionary tracks using the full posterior distribution from forward modeling the effective temperature and surface gravity with PHOENIX atmospheric models. The bimodal mass distribution corresponds to a bimodal temperature distribution in the forward-model posterior. (b) The same posterior corresponds to a radius of 1.08﹩{}_{-0.04}^{+0.05}﹩ RJup.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Corner plot for HD 206893 B showing effective temperature, surface gravity, ﹩v\sin i﹩, and RV using the BT-Settl (F. Allard et al. 2012) model grid and the KPIC K-band spectra. The corner plot shows a bimodal distribution in spin and RV.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: (a) Interpolated age and mass distributions while limiting the temperature prior space to below 1750 K. The bimodality of the mass distribution disappears in this temperature range while the age of the object remains constant with the full model grid. (b) The bimodal mass distribution shifts to the lower-mass value, while the radius increases slightly, though still consistent with the full grid.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: The walker plot for both ﹩v\sin i﹩ and RV from 14. The MCMC has converged to a bimodal distribution based on the density of the walker traces.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Semimajor axis and eccentricity over time for random draws for HD 206893 B and c for 1 Myr integration. We find that there is no strong preference for circular/elliptical orbits or specific semimajor axis values. Configurations are stable in about ∼95.8% of cases.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Semimajor axis and eccentricity over time for HD 206893 B and c for 1 Gyr integration. We find that there is a strong preference for circular orbits and for a larger semimajor axis for B and c. Configurations are stable in ∼0.8% of cases.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Corner plot generated by petitRADTRANS retrieval fitting GPI J-band, H-band, and K-band data simultaneously from K. Ward-Duong et al. (2021).
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Same as Figure 16, but only fitting using H-band data.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Same as Figure 16, but only fitting using J-band data.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: (a) χ2 contour plot for fits to the CO2 emission, as a function of temperature and CO2 column density. The white solid contour lines mark 1σ, 2σ, and 3σ confidence intervals on the best-fit model, shown with a white star. The dashed yellow lines show best-fit emitting radii (R) corresponding to each model. (b) Line peak ratio of the Q branches of 12CO and 13CO, assuming 12C/13C = 68. The yellow lines show the observed ratio of 2.24 ± 0.24. (c) Line peak ratio of the Q branches of 12CO and C18O16O, assuming 12CO/C18O16O = 278.5. The yellow lines show the observed ratio of 2.97 ± 0.36.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Continuum-subtracted MIRI-MRS spectrum of MY Lup (black) and Keck-NIRSPEC spectrum of weak-line T Tauri star TWA 7 (blue), convolved to a resolving power of R = 3000 and scaled to visually match the MY Lup spectrum. Regions of the TWA 7 spectrum with high telluric contamination have been removed.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Observed MIRI-MRS spectrum of MY Lup (black, top), continuum fit (blue), and continuum-subtracted flux (black, bottom). Prominent atomic and molecular emission features are labeled; S(X) refers to H2 0–0 transitions. The broad feature at 10 μm is the emission from solid silicates. The insets show continuum-subtracted spectra in the regions with significant HCN, CO2, and OH emission; the vertical bars also highlight the locations of the main Q branches for different isotopologues.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: MY Lup MIRI-MRS continuum-subtracted and water-model-subtracted spectrum in the CO2-emitting region (black), plus slab emission models for CO2 and isotopologues (various colors) assuming a C ratio fixed to the ISM value—see Table 1 for model parameters. The location of the marginal C17O16O detection is highlighted with a brown triangle. [Ne III] emission at 15.555 μm is also marked. Residuals (data – model) are shown in gray, offset by 0.01 Jy for clarity. The large residual at ∼14.99 μm is discussed further in Appendix B.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Portions of the continuum-subtracted MY Lup MIRI-MRS spectrum (black) and slab water emission model (blue) with T = 336 K, N = 9.9 × 1017 cm−2, and R = 1.20 au. The gray dashed lines mark the locations of the water lines used in the MCMC fit; note that rovibrational emission at 7 μ is not included in the fit. H2 and H I emission lines are also marked.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Line images of [Ne II], H2 S(1), 12CO2, and a combination of five H2O emission lines near 17 μm. The circles mask an inner working angle of 1 × 1.22 λ/D around the star. The yellow contours show the ALMA continuum from S. M. Andrews et al. (2018; the contours mark 5σ, 50σ, and 100σ).
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Observed continuum-subtracted MY Lup spectrum (black), best-fit slab water model convolved to an FWHM of 120 km s−1 (blue), and residuals (gray, offset) in the HCN- and CO2-emitting regions. The vertical bars mark the same molecular Q branches highlighted in Figure 1.
Paper: The Baryonic Tully–Fisher Relation. II. Stellar Mass Models
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: Updated ϒ* models from SML. The three models shown (discussed in the main text) represent pure bulge and disk SFHs, which are then combined to produce a bulge + disk (“B + D”) scenario guided by the main-sequence relation (J. S. Speagle et al. 2014) and a chemical enrichment model. Standardized to the g − W1 or g − [3.6] color, at the 3.5 μm wavelength the difference between ϒ* is only larger by 10% from IRAC 3.6 μm to WISE W1.
Paper: The Baryonic Tully–Fisher Relation. II. Stellar Mass Models
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: Using the models from Figure 1, the IRAC 3.6 μm and WISE W1 total luminosities are converted into total stellar masses in an independent fashion. Due to the typically redder and narrow range of W1 − [3.6] colors plus only slightly higher ϒ* values, it is unsurprising to find the relationship between stellar mass at W1 and 3.6 μm has a slope of 1. The error from a slope of unity is ±0.01 and the scatter is completely explained by photometric errors. The red and green symbols are 20 and 16 galaxies in common from the S4G and Dustpedia surveys, respectively. The residual diagram at the bottom shows no systematics over the range of stellar masses with a mean offset of 0.02 ± 0.18 dex.
Paper: The Baryonic Tully–Fisher Relation. II. Stellar Mass Models
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: A comparison of stellar masses deduced by g − W1 colors (SPARC) vs. W1 − W2 color relation (M. E. Cluver et al. 2014). The WISE sample was selected for only those galaxies in the SPARC sample with W2 fluxes with a signal-to-noise ratio (S/N) greater than 20. Typical errors in the stellar mass are shown and the rms for the comparison of 58 galaxies is 0.29 in log scale. The right panel displays the log LW1 vs. stellar mass relationship outlined in T. H. Jarrett et al. (2023; magenta line, a polynomial fit to the GAMA masses). Our WISE models are shown as a red band of ±0.2 dex error width based on a g − W1 color–magnitude relation to obtain LW1. The dashed line indicates a constant ϒ* = 0.35.
Paper: The Baryonic Tully–Fisher Relation. II. Stellar Mass Models
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: A comparison of W1 luminosity vs. gas fraction, Mgas/Mbar, for the WISE SPARC sample. The left panel displays gas fractions using the color relation presented in this paper, while the right panel uses a constant value of 0.2 proposed by T. H. Jarrett et al. (2023). Hubble types are indicated such that early-type spirals are red symbols, Sc’s are green, and late-type dwarfs are blue. The prediction of gas fraction as a function of luminosity from the Illustris-TNG50 galaxy formation simulations (M. Korsaga et al. 2023) is shown as a magenta line.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: Examples of Class A (left panels) and Class B (right panels) OCs. The subplots display various aspects of the member stars. Panels (a) shows the member stars in Galactic coordinates. Panels (b) presents the density profile along with the corresponding King model fitting, highlighting the boundary radius rb. Specifically, CWNU 3455 is a newly identified OC from H23, situated within the Galactic northern warp. This cluster exhibits a high concentration of member stars. In contrast, CWNU 3593 displays poor concentration, resulting in the King model’s failure to accurately fit its density profile. Panels (c) depicts the various star types on the H-R diagram. Gray dots represent the stars with a membership probability greater than 50%. Black dots indicate core (larger) and border (smaller) member stars. Large and small blue squares denote BSS candidates among core and border members, respectively. The purple dashed line marks the ZAMS, while the brown and gray dashed line illustrates the best-fit isochrone line and its binary sequence, respectively. The full figure sets for other 51 OCs can be seen in Appendix A.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: (a) Distribution of Type I and Type II BSSs relative to Me. (b) Mass of Type I BSSs (MBSS) vs. the TO mass of the cluster (MTO). The brown solid and dotted lines signify the fractional mass excess Me = 1 and Me = 0.5, respectively. (c) Me of Type I BSSs plotted against cluster age. (d) Me of Type I BSSs plotted against cluster mass (logarithmic mass/M⊙). The color of the scatter points reflects the degree of spatial density in the distribution. Warmer colors signify a greater degree of crowding among the data points.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: Left panels: the mass of OCs plotted against various age ranges. The black line represents the median logarithmic mass/M⊙ within each age range. Right panels: the maximum fractional mass excess of OC BSSs in different age ranges presented as a function of cluster mass. The dashed lines illustrate the running median values of maximum Me in relation to cluster mass. The triangles indicate OCs containing Type 1 BSSs identified in this study, while solid circles denote BSSs cataloged in V. V. Jadhav & A. Subramaniam (2021). The brown solid and dotted lines correspond to Me = 1 and Me = 0.5, respectively. The colors indicate scatter point density, with cooler colors representing sparse areas and warmer colors indicating crowded areas.