adsabs/AstroCLIMB huggingface dataset:
Paper: Search for Past Stellar Encounters and the Origin of 3I/ATLAS
Authors: Yiyang Guo, Luyao Zhang, Fabo Feng, Zhao-Yu Li, Anton Pomazan, Xiaohu Yang
Figure caption: Distributions of nominal and median encounter distances ﹩{d}_{{\rm{enc}}}^{}﹩ and encounter speeds ﹩{v}_{{\rm{enc}}}^{}﹩ for encounters with each 95% quantile of ﹩{d}_{{\rm{enc}}}^{}﹩ below 1.5 pc. The left panel represents the nominal values of ﹩{d}_{{\rm{enc}}}^{{\rm{nom}}}﹩ and ﹩{v}_{{\rm{enc}}}^{{\rm{nom}}}﹩. The right panel represents median values of ﹩{d}_{{\rm{enc}}}^{{\rm{med}}}﹩ and ﹩{v}_{{\rm{enc}}}^{{\rm{med}}}﹩. Error bars indicate 5% and 95% quantiles of ﹩{d}_{{\rm{enc}}}^{}﹩ and ﹩{v}_{{\rm{enc}}}^{}﹩ in MC results. The color bar is based on Equation (3) using the median of g.
Paper: Search for Past Stellar Encounters and the Origin of 3I/ATLAS
Authors: Yiyang Guo, Luyao Zhang, Fabo Feng, Zhao-Yu Li, Anton Pomazan, Xiaohu Yang
Figure caption: Histograms of relative speeds of 3I/ATLAS and ∼134,000 nearby stars with radial velocities.
Paper: Search for Past Stellar Encounters and the Origin of 3I/ATLAS
Authors: Yiyang Guo, Luyao Zhang, Fabo Feng, Zhao-Yu Li, Anton Pomazan, Xiaohu Yang
Figure caption: Comparison of two encounter MC results. In both panels, the orange dots represent one 3I/ATLAS nominal sample and 200 star MC samples' pairwise results, while the purple dots represent 1000 3I/ATLAS MC samples and 1 star nominal sample pairwise results.
Paper: Search for Past Stellar Encounters and the Origin of 3I/ATLAS
Authors: Yiyang Guo, Luyao Zhang, Fabo Feng, Zhao-Yu Li, Anton Pomazan, Xiaohu Yang
Figure caption: Cumulative speed change Δv and deflection angle δ.
Paper: Search for Past Stellar Encounters and the Origin of 3I/ATLAS
Authors: Yiyang Guo, Luyao Zhang, Fabo Feng, Zhao-Yu Li, Anton Pomazan, Xiaohu Yang
Figure caption: Distributions of deflection angle δ and g smoothed with a Gaussian kernel.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Precision diagnostics as a function of separation ρ (arcsec): (a) angular uncertainty σθ (deg) vs. ρ; (b) radial uncertainty σρ (mas) vs. ρ; (c) tangential component ρσθ (mas) vs. ρ with an origin-constrained linear fit (y = a x) and an ∼95% precision band; (d) photometric uncertainty σΔm (mag) vs. ρ. Panels (a), (b), and (d) show the binned median (line) and the interquartile range (shaded band). All panels share the same x-axis in arcseconds; x-labels are displayed only on the bottom row.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Box plot showing the percentage reduction in the uncertainties of separation (ρ), position angle (θ), tangential coordinate (ρσθ), and magnitude difference (ΔmR) after applying PCA and bicubic interpolation. Each box represents the distribution of reductions across the observed binary systems, highlighting the consistent improvement in measurement precision, especially for ρ.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Autocorrelation function of WDS 00550+2338. Top: original ACF without interpolation; separation ﹩\rho =1\mathop{.}\limits{^{\prime\prime} }19\pm 0\mathop{.}\limits{^{\prime\prime} }01﹩. Bottom: ACF after PCA filtering, bicubic interpolation, and central masking; separation ﹩\rho =1\mathop{.}\limits{^{\prime\prime} }189\pm 0\mathop{.}\limits{^{\prime\prime} }005﹩. The secondary peaks become smoother and more symmetric, and their contrast relative to the background is improved.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Top: zoomed ACF of WDS 01072+3839 before applying a circular central mask, isolating the main companion peak (pixel units). Bottom: detection of the secondary star’s local maxima. This is a detection-only diagnostic in pixel units; no calibrated astrometry shown. The separation at the epoch is omitted here and reported in Figures 3 and 5 after applying pixel-scale and orientation calibrations.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Top: PWS comparison of WDS 00550+2338 before (left) and after (right) PCA processing; separation ﹩\rho =1\mathop{.}\limits{^{\prime\prime} }189\pm 0\mathop{.}\limits{^{\prime\prime} }005﹩. Bottom: same comparison for WDS 01072+3839; separation ﹩\rho =0\mathop{.}\limits{^{\prime\prime} }130\pm 0.004﹩.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Cumulative variance recovered as a function of the number of retained PCA components. Most of the signal is captured within the first 50–100 components, justifying the 99% cutoff used in our reduction pipeline.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Zoomed region around the companion peaks in the ACF of WDS 01072+3839, after central masking and bicubic interpolation resampling. Separation ﹩\rho =0\mathop{.}\limits{^{\prime\prime} }130\pm 0.004﹩.
Paper: PCA-enhanced Speckle Interferometry with Bicubic Interpolation at the OAN-SPM México
Authors: C. A. Guerrero, D. O. Ochoa, B. Hernández-Valencia, T. Benadalid, I. A. Peralta-Mendoza, E. Romero Hernández, F. A. García-Castillo, S. Ayala, J. E. Pérez-León, F. J. Tamayo, A. Avilés, E. Sánchez, J. H. Castro-Chacón, A. Bautista-Hernández, M. Reyes-Ruiz, E. G. Pérez-Tijerina
Figure caption: Stages of the automatic detection process using maximum filtering and masking on the interpolated ACF. Gaussian centroid refinement is applied to the final detections.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: The PAR for the 41 F mode and 1O mode OC Cepheids, compared with those derived by G. Bono et al. (2005), Anderson16, and ZC21. Red and blue points represent 41 OC Cepheids from this work; blue points appear in the ZC21 PAR sample, while red points are newly identified outside of ZC21. Gray filled points and open circle are candidates or rejected samples in this work that are the other part of the PAR fitting samples in ZC21. One outlier is shown as a red open circle.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: CMDs of the four newly identified OC Cepheids are shown, including the extinction, age, and distance parameters of their host clusters: Bochum 14, Theia 358, FSR 0158 (NSVS 8389949), and CWNU 3123. In each CMD, black points represent cluster member stars, and the inset shows the spatial distribution of members in Galactic coordinates. The size of the black points indicates the membership reliability of cluster stars as reported by He23: larger points correspond to high-confidence member stars, while smaller points represent candidate members. The blue shaded region indicates the age uncertainty, while the dark blue line corresponds to the ﹩\mathrm{logAge}﹩ derived from isochrone fitting. Astrometric dispersions (δϖ and δpm), parallax, extinction, and age values are provided in each panel.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: Comparison of the cluster ages and extinctions obtained from the isochrone fitting with those from the literature, including CG20, Dias21, He22, He23, and HR24. Points of different colors correspond to OCs from the respective references.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: The PWR of 41 OC Cepheids, including both F and 1O mode pulsators. Red points represent the newly identified samples from this work, black points denote previously confirmed samples, and one open circle indicates the outlier. The fitted relations are compared with those from ZC21, Lin22, CRA23, and V. Ripepi et al. (2023).
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: Comparison of OC age determinations using different PARs. The upper panels compare cluster ages and CC period distributions from CG20, Dias21, and HR24. In the lower panels, red, green, and blue points represent the age residuals relative to the PAR fits from this work, Anderson16, and ZC21, respectively. The corresponding weighted mean residuals are indicated by the red, green, and blue lines.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: Period–age distribution of OC Cepheid candidates and rejected samples. Red points represent OC Cepheid candidates, while black points indicate the rejected samples. The black line represents the PAR derived in this work.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: CMDs of the remaining part of OC Cepheids, which also contain the extinction, age, and distance parameters of the OCs, namely, NGC 103, CWNU 2461, NGC 6664, Kronberger 84 (J213533.70+533049.3), CWNU 2232, HSC 2354, Theia 3005, CWNU 2478, NGC 7790 (CE Cas B), UBC 229, NGC 7790 (CF Cas), NGC 7790 (CE Cas A), CWNU 175, vdBergh 1, NGC 5662, HSC 413, UBC 1429, UBC 135, Berkeley 55, and Ruprecht 79.