adsabs/AstroCLIMB huggingface dataset:
Paper: Statistical Properties of Solar Wind and Interplanetary Magnetic Field Upstream of Planets at 1 au and Beyond: A Comprehensive Analysis
Authors: Tao Tang, Ruilong Guo, Quanqi Shi, Jong-Sun Park, Xiao Ma, Jinyan Zhao, Xuzhi Zhou, Hui Zhang, Limei Yan, Anmin Tian, Shichen Bai, Yijia Zhou, Alexander William Degeling, Yuchen Xiao, Qiugang Zong
Figure caption: Distribution of solar wind parameters upstream of Mars: (a) V, (b) Np, and (c)–(d) Bx and IMF projections in the MSO coordinate system XY plane, constrained to MAVEN’s Z-position (−1.2 RM < Zmso < 1.2 RM, RM is Mars radius). Panels (c) and (d) categorize IMF directions into (c) outward (By > 0) and (d) inward (By < 0) sectors. The black and white hemispheres correspond to the nightside and dayside of Mars, respectively. The red curves in each panel represent the average position of the Martian bow shock at Z = 0 (J. R. Gruesbeck et al. 2018). The black curves in panels (a) and (b) represent the quadratic function curves: x = −y2/5 + 2.1, which divide the solar wind data upstream of Mars into two parts: close to the bow shock and far from the bow shock. The black arrows in panels (c)–(d) represent the averaged IMF magnitude and direction in the XY plane. The average in each bin (grid size of 0.3 RM × 0.3 RM) is color coded according to the color bar on the right-hand side of each panel.
Paper: Statistical Properties of Solar Wind and Interplanetary Magnetic Field Upstream of Planets at 1 au and Beyond: A Comprehensive Analysis
Authors: Tao Tang, Ruilong Guo, Quanqi Shi, Jong-Sun Park, Xiao Ma, Jinyan Zhao, Xuzhi Zhou, Hui Zhang, Limei Yan, Anmin Tian, Shichen Bai, Yijia Zhou, Alexander William Degeling, Yuchen Xiao, Qiugang Zong
Figure caption: The statistical distributions of B (first column), Np (second column), V (third column), and Tp (fourth column) upstream of Earth (first row), Mars (second row), and Saturn (third row) during solar maximum (red bars) and solar minimum (blue bars). The sample size is denoted by N. The mean (solid line) and median (dashed line) are indicated in each panel. The black p-values in each panel indicate the results of Welch’s t-test for mean comparisons, while the brown p-values represent the Mann–Whitney U test results for median comparisons.
Paper: Statistical Properties of Solar Wind and Interplanetary Magnetic Field Upstream of Planets at 1 au and Beyond: A Comprehensive Analysis
Authors: Tao Tang, Ruilong Guo, Quanqi Shi, Jong-Sun Park, Xiao Ma, Jinyan Zhao, Xuzhi Zhou, Hui Zhang, Limei Yan, Anmin Tian, Shichen Bai, Yijia Zhou, Alexander William Degeling, Yuchen Xiao, Qiugang Zong
Figure caption: The statistical distribution of IMF θa (first column), V (second column), β (third column), and MA (fourth column) upstream of Earth (first row), Mars (second row), Jupiter (third row), and Saturn (fourth row) during solar descending (green bars) and solar ascending (purple bars) phases. The sample size is denoted by N. The mean (solid line) and median (dashed line) are indicated in each panel. The black p-values in each panel indicate the results of Welch’s t-test for mean comparisons, while the brown p-values represent the Mann–Whitney U test results for median comparisons.
Paper: Statistical Properties of Solar Wind and Interplanetary Magnetic Field Upstream of Planets at 1 au and Beyond: A Comprehensive Analysis
Authors: Tao Tang, Ruilong Guo, Quanqi Shi, Jong-Sun Park, Xiao Ma, Jinyan Zhao, Xuzhi Zhou, Hui Zhang, Limei Yan, Anmin Tian, Shichen Bai, Yijia Zhou, Alexander William Degeling, Yuchen Xiao, Qiugang Zong
Figure caption: The statistical distributions of the alpha ratio upstream of (a), (b) Earth, and (c) Jupiter during different solar activity phases: solar maximum (red bars), solar minimum (blue bars), solar descending phase (green bars), and solar ascending phase (purple bars). The sample size is denoted by N. The mean (solid line) and median (dashed line) are indicated in each panel. The black p-values in each panel indicate the results of Welch’s t-test for mean comparisons, while the brown p-values represent the Mann–Whitney U test results for median comparisons.
Paper: Statistical Properties of Solar Wind and Interplanetary Magnetic Field Upstream of Planets at 1 au and Beyond: A Comprehensive Analysis
Authors: Tao Tang, Ruilong Guo, Quanqi Shi, Jong-Sun Park, Xiao Ma, Jinyan Zhao, Xuzhi Zhou, Hui Zhang, Limei Yan, Anmin Tian, Shichen Bai, Yijia Zhou, Alexander William Degeling, Yuchen Xiao, Qiugang Zong
Figure caption: The statistical distribution of Pdyn (first column), β (second column), E (third column), and VA (fourth column) upstream of Earth (first row) and Mars (second row) during solar maximum (red bars) and solar minimum (blue bars). The sample size is denoted by N. The mean (solid line) and median (dashed line) are indicated in each panel. The black p-values in each panel indicate the results of Welch’s t-test for mean comparisons, while the brown p-values represent the Mann–Whitney U test results for median comparisons.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: CMD and the corresponding density distributions for the identified SB2 candidates and SB2 candidates from M. Kovalev et al. (2024b). The vertical axis shows the G-band absolute magnitude, calculated by the equation: ﹩{M}_{G}=G\,{\rm{-band apparent magnitude}}\,+5+5{{{\mathrm{log}}}_{10}}\,(\,{\rm{parallax}}\,/1000)﹩, while the horizontal axis shows the GBP − GRP color. The right and top panels depict the KDE curve of G-band absolute magnitude and GBP − GRP color.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Comparison of the RVs estimated by above method with the RVs provided by S.-s. Li et al. (2025). The left and right panels respectively show the comparison results of RV1s and RV2s, arranged in ascending order of their values. Each subplots is colored by data density fitted by the KDE method with a gray dashed line representing the identity line.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Typical CCF examples of sample data sets. The top left and top right panels show the positive samples. The bottom left and bottom right panels show the negative samples.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: The distribution of RV measurement errors. Markers are colored by snr. The measurement errors of RV1 and RV2 are represented by the horizontal and vertical coordinates, respectively, arranged in ascending order of their values.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: The prediction uncertainty distributions of SB2Net. The left panel shows the KDE curve of epistemic uncertainty across the test set, while the right panel depicts the KDE curve of aleatoric uncertainty on the same set.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Example of spectrum normalization. The top panel shows the original spectrum with fitted continuum. The bottom panel is the spectrum after normalization.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Confusion matrix of SB2Net based on the test set.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Overview of SB2Net architecture with details of ACAM and GRU. After data processing, the CCF is input into the SB2Net, where it first passes through a convolutional layer, a layer normalization layer, and a Gaussian error linear unit activation function to increase the number of channels. Subsequently, feature extraction is performed by the NRCA module consisting of four NRCA blocks. Each NRCA block is composed of two convolutional layers, two layer-normalization layers, two Gaussian error linear unit activation functions, and an ACAM, as illustrated in the bottom left panel. Additionally, the LSD module, consisting of five stacked GRUs, simulates the sequential dependencies of the CCF and extracts global sequence information, as illustrated in the bottom right panel. The output module produces the model’s final classification results, consisting of a flatten layer, a MC dropout layer, and two linear layers. During the forward propagation, the model computes the loss, while during the backward propagation, it calculates gradients and updates parameters to optimize the prediction performance.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: The eccentricity e and mass ratio q as a function of period p, colored by absolute magnitude. Left panel: Period–eccentricity diagram of the well-fitted systems. The red dashed line represents the upper envelope of eccentricity from T. Mazeh (2008) through the statistics of binaries in the ﹩{S}_{{\,{\rm{B}}\,}^{9}}﹩. Right panel: Relationship between mass ratio and period. The solid black line and dotted black line represent q = 1 and q = 0.1, respectively.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Example of a well-fitted orbit. The top panel displays the RV curves of the primary (solid blue line) and secondary (dashed red line) star. The bottom two panels show the residuals of the fit for primary and secondary star, respectively.
Paper: Double-lined Spectroscopic Binaries Identified in LAMOST DR11 with a Deep Learning Model
Authors: Ke Wang, Yude Bu, Yuhang Zhang, Mengmeng Zhang, Shanshan Li, Jiangchuan Zhang, Huili Wu, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Distribution of samples predicted as SB2s by the model in the entire sky. Gray dots represent target sources within the LAMOST observation range, blue dots represent candidates discovered in this study that have already been reported by other catalogs, and purple dots represent newly discovered candidates in this study.
Paper: Parkes Transient Events. II. Pulsar Single-pulses Database Containing Raw Data Segments
Authors: Xuan Yang, Songbo Zhang, Le-Yu Tang, L. Toomey, Xuefeng Wu
Figure caption: The process executed by the script GET_PULSAR_PUB.PY: it first extracts the blob data from the PTD II (left), subsequently saves this data as a PSRFITS file (middle), and finally generates a plot of the single pulse using the PSRFITS file (right). Top to bottom on the right side shows an integrated pulse profile using an arbitrary flux density scale, the time–frequency plane, an integrated pulse profile after being dedispersed at the pulsar DM, and a single-pulse spectrum after being dedispersed at the pulsar DM. The narrow blue lines with short red lines on the left side are the marked narrowband radio-frequency interferences.
Paper: Parkes Transient Events. II. Pulsar Single-pulses Database Containing Raw Data Segments
Authors: Xuan Yang, Songbo Zhang, Le-Yu Tang, L. Toomey, Xuefeng Wu
Figure caption: Fluence of 3672 single pulses of PSR J0942–5552 from five observation epochs. The x-axis represents the pulse-train number relative to the start of the observation, measured in units of the rotating period (P0). Each observation epoch is indicated by a blue background. The red solid lines represent the rms level variation scaling to mean fluence level.
Paper: Parkes Transient Events. II. Pulsar Single-pulses Database Containing Raw Data Segments
Authors: Xuan Yang, Songbo Zhang, Le-Yu Tang, L. Toomey, Xuefeng Wu
Figure caption: Fluence of 2066 single pulses of PSR J1602–5100 from four observation epochs. The x-axis represents the pulse-train number relative to the start of the observation, measured in units of the rotating period (P0). Each observation epoch is indicated by a blue background. The red solid lines represent the rms level variation scaling to mean fluence level.
Paper: Parkes Transient Events. II. Pulsar Single-pulses Database Containing Raw Data Segments
Authors: Xuan Yang, Songbo Zhang, Le-Yu Tang, L. Toomey, Xuefeng Wu
Figure caption: Fluence of 3516 single pulses of PSR J1745–3040 from two observation epochs. The x-axis represents the pulse-train number relative to the start of the observation, measured in units of the rotating period (P0). Each observation epoch is indicated by a blue background. The red solid lines represent the rms level variation scaling to mean fluence level.
Paper: Parkes Transient Events. II. Pulsar Single-pulses Database Containing Raw Data Segments
Authors: Xuan Yang, Songbo Zhang, Le-Yu Tang, L. Toomey, Xuefeng Wu
Figure caption: Fluence of 214 single pulses of PSR J1539–5626 from three observation epochs. The x-axis represents the pulse-train number relative to the start of the observation, measured in units of the rotating period (P0). Each observation epoch is indicated by a blue background. The red solid lines represent the rms level variation scaling to mean fluence level.
Paper: Parkes Transient Events. II. Pulsar Single-pulses Database Containing Raw Data Segments
Authors: Xuan Yang, Songbo Zhang, Le-Yu Tang, L. Toomey, Xuefeng Wu
Figure caption: The fluence ratio distribution of the 363 pulsars.
Paper: Parkes Transient Events. II. Pulsar Single-pulses Database Containing Raw Data Segments
Authors: Xuan Yang, Songbo Zhang, Le-Yu Tang, L. Toomey, Xuefeng Wu
Figure caption: Chart of the database schema.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: A comprehensive collection of orbital solutions from this work; the results from previous detailed studies that would otherwise have been in our sample are also included for completeness. Very close-in, low-mass planets lie outside the axis limits. Top: companion masses and semimajor axes, color coded by orbital eccentricity. Marker size indicates the uncertainty in eccentricity (σe), with larger markers corresponding to better-constrained eccentricities. Blue lines separate stellar, brown dwarf, and planetary-mass companions. Red upward-pointing arrows denote companions with minimum mass constraints (﹩{M}_{2}\sin {}i﹩). The histogram of companion masses is shown to the right, with the brown dwarf desert highlighted around 25–65 MJup. (Bottom) Same as the top panel, but for mass ratio (M2/M1). The brown dwarf desert appears to be slightly more pronounced.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: (Top left) RV time series of HIP 3850 (=HD 4747), showing substantial phase coverage of the orbit. These RVs provide enough information to derive a full orbit solution when combined with astrometric data. (Top right) RV time series of HIP 108870, illustrating packed RV observations. The measurements are closely clustered in time, reducing the number of effectively distinct observational epochs and limiting the available orbital information. (Bottom) RV time series of HIP 110109, showing a straight-line trend. This trend suggests the absence of detectable curvature, making it challenging to derive a complete orbital solution without the aid of relative astrometry.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: Corner plot of the orbital elements of HIP 106440 b, illustrating the posterior distributions and correlations among the parameters and orbital inclination. In the lower-right 1D histograms, the vertical dashed lines around the central dashed line indicate the 16% and 84% quantiles. In the 2D histograms, the contours correspond to the 1σ, 2σ, and 3σ equivalent uncertainties. The inclination distribution is bimodal, with peaks near 55° and 125°, symmetric about 90°. This reflects the degeneracy in distinguishing between prograde and retrograde orbits.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: Combined posterior distribution of orbital inclinations from every orvara chain in our sample. Gray bars show the histogram of ∼1.6 × 106 MCMC samples (both inc0 and inc1 if there are two companion fitted), binned in 4﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 intervals. The red curve is the theoretical probability density ﹩(1/2)\sin i﹩—scaled to the same total number of samples and bin width—that describes an isotropic ensemble of orbital inclinations. This figure confirms that our joint RV + absolute/relative astrometry selection and fitting introduces little systematic bias toward extreme inclination orbits.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: Top: relative orbits of HIP 12436 Ab (in arcseconds), fit jointly to RVs and absolute astrometry. We show 50 random draws from the MCMC orbit distribution, color coded by companion mass, with the black curve representing the maximum-likelihood solution. The star symbol at the origin marks the host star, and selected epochs along the maximum-likelihood orbit are annotated. Bottom: observed RVs of HIP 12436 overplotted with the best-fit orbital solution (black) and a random sampling of orbits from the MCMC chain. Residuals from the best-fit orbit appear in the lower subpanel.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: Observed RVs of HIP 39417, plotted with the best-fit orbital model (black) and random draws (color coded by mass of HIP 39417 c) from the MCMC chain. The short-term deviations primarily constrain the inner planet b, while the limited long-term coverage shapes the outer planet c.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: Observed RVs of HIP 21865, plotted with the best-fit orbital model (black) and random draws from the MCMC chain. The lower subpanel shows the residuals relative to the best-fit orbit. The HARPS fiber swap in 2015, unfortunately, limits the constraining power of the data.
Paper: Orbits and Masses for 156 Companions from Combined Astrometry and Radial Velocities, and a Validation of Gaia Non-single-star Solutions
Authors: Qier An, Timothy D. Brandt, G. Mirek Brandt, Alexander Venner
Figure caption: Observed RVs of HIP 19428, plotted alongside the best-fit orbital solution (black) and random orbits from the MCMC chain. The lower subpanel presents the residuals relative to the best-fit orbit.
Paper: The Period–Luminosity Relation of Long-period Variables in the Large Magellanic Cloud Observed with ATLAS
Authors: Daniel Hey, John Tonry, Benjamin Shappee, Daniel Huber
Figure caption: Top: The period–luminosity relation for the stars in the LMC sample with amplitude as measured in the ATLAS o band. We show only the dominant period of variability, which we define as that of the highest amplitude. Note the white strips comprising removed systematics near the lunar synodic period (∼29 days) and integer multiples thereof. Bottom: The same PL relation after only selecting high-probability members as discussed in Section 4.2. Note that this selection still retains a handful of systematic contaminants at short periods. Individual sequences are fit as discussed in the text.
Paper: The Period–Luminosity Relation of Long-period Variables in the Large Magellanic Cloud Observed with ATLAS
Authors: Daniel Hey, John Tonry, Benjamin Shappee, Daniel Huber
Figure caption: The LMC PL relation colored by the ratio of the dominant period amplitudes measured in the ATLAS cyan and orange passbands.
Paper: BASSET: Bandpass-adaptive Single-pulse Search Toolkit—Optimized Subband Pulse Search Strategies for Faint Narrowband Fast Radio Bursts
Authors: J. H Cao, P. Wang, D. Li, Q. H. Pan, K. Mao, C. H. Niu, Y. K. Zhang, Q. Y. Qu, W. J. Lu, J. S. Zhang, Y. H. Zhu, Y. D. Wang, H. X. Chen, X. L. Chen, J. H. Fang, Y. Feng, H. Gao, Y. F. Huang, J. Li, C. C. Miao, C. W. Tsai, J. M. Yao, S. P. You, R. S. Zhao, Q. Z. Liu, S. M. Weng, S. H. Yew, J. Zhang, L. Zhang, E. Gügercinoğlu, D. K. Zhou, W. W. Zhu
Figure caption: The performance of BASSET when applied to a series of morphologically complex pulses from FRB 20201124A. Panel (a) shows the SNRB/SNRA. In panel (b), the blue dashed line represents the time series processed by the standard pipeline, and the orange solid line represents the time series processed by BASSET. The gray dashed line marks the SNRA = 10 threshold, and the region where SNRA > 10 is shaded. This time region represents the time location of the pulses identified by the standard pipeline. No frequency localization is provided, as the standard pipeline averages the data across all frequency bands. Panel (c) shows the dynamic spectrum of the pulses. The time–frequency regions searched by BASSET are highlighted with red boxes. The frequency channels affected by RFI are masked and highlighted.