adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Top left panel: exposure count histogram. The subplot displays a cumulative bar chart of exposure counts. Top right panel: EWHα coefficient of variation histogram. Bottom left panel: Δ EWHα histogram. The subplot shows an enlarged view of the portion where Δ EWHα is greater than 0.4. Bottom right panel: relationship between Spectral Type and max(﹩{{\rm{EW}}}_{{\rm{H}}\alpha }^{{\prime} }﹩)/min(﹩{{\rm{EW}}}_{{\rm{H}}\alpha }^{{\prime} }﹩). The red dots represent the median values of the data for stars of different spectral types. The upper panel is a zoomed-in view around the median, provided to better illustrate the variations.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Left panel: relationship between logg and Teff, with the black dashed line indicating the boundary between giants and main-sequence stars (D. R. Ciardi et al. 2011). The color bars represent [Fe/H]. Middle panel: density distribution plot of Teff and logg. The color bar represents the number density. Right panel: color–magnitude Hertzsprung–Russell diagram. The color bar represents the number density.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: The first column of the panel depicts the relationship between logRo and log﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩. The second column shows the relationship between logProt and log﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩. The color bars for all panels represent Teff. The gray error bars represent the y-axis errors. The red solid lines in all panels represent the fitting results for each data set, while the red shaded areas show the 3σ regions of the fitting results.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Left panel: relationship between Teff and EWHα. The color bar represents logg. The solid red line represents a fourth-degree polynomial fit for the least active 2% of stars in each temperature bin, with 100 bins. Right panel: relationship between Teff and ﹩{{\rm{EW}}}_{{\rm{H}}\alpha }^{{\prime} }﹩. The color bar represents the number density. The black dashed line represents y = 0. The black dashed–dotted line connects the median in each Teff bin, with 500 bins.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Comparison of the stellar rotation periods obtained in this work with other studies. In the figure, the red, green, and blue solid lines represent x = y, x = 2y, and x = 1/2y, respectively. The shaded regions in corresponding colors indicate ± 10% errors for each line.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Statistical histograms of various spectral types of log﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩. The solid orange line in the figure represents the Gaussian fit results. The dashed blue line indicates the corresponding x-axis values of the Gaussian fit peaks.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Left panel: ﹩{{\rm{R}}}_{{\rm{H}}\alpha }^{{\prime} }﹩ histograms for flaring and nonflaring stars of various spectral types. The blue solid line represents the Gaussian fitting results for nonflaring stars, and the red solid line represents the Gaussian fitting results for flaring stars. The dashed lines in corresponding colors indicate the peaks of the Gaussian fits. The shaded area corresponding to the color represents the error of the corresponding Gaussian fit. Right panel: Scatter plots of Teff–﹩{{\rm{EW}}}_{{\rm{H}}\alpha }^{{\prime} }﹩ and Teff–﹩{{\rm{R}}}_{{\rm{H}}\alpha }^{{\prime} }﹩ for flaring and nonflaring stars. Red dots represent flaring stars, and gray dots represent nonflaring stars. The yellow dashed line shows the median value for each bin of flaring stars, and the blue dashed line shows the median value for each bin of nonflaring stars. The bin size is 500.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: These panels show the relationship between flare energy and duration for M-type and F-type stars across different effective temperature ranges. The red solid line in the plot represents the best-fit line. The green shaded area represents the ± 1σ deviation of each data point from the fitted line, the gray shaded area represents the ± 3σ deviation of each data point from the fitted line.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: These panels show the relationship between flare energy and duration for stars of different spectral types. Unlike Figure 10, these images do not include giant star samples, and the vertical axis represents the logarithm of the duration. The red solid line in the plot represents the best-fit line. The green shaded area represents the ± 1σ deviation of each data point from the fitted line, the gray shaded area represents the ± 3σ deviation of each data point from the fitted line.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: These panels show the relationship between flare energy and duration for stars of different spectral types. The color bar indicates the number density. The red solid line in the top middle panel divides the data points into two parts, with all the data points on the right side representing results from giant stars.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: These panels display the proportion of flaring stars for different temperatures, masses, and spectral types.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: The first and third columns display the spectra of the Hα line for individual stars. The second and fourth columns show the relationship between observation time and EWHα for the corresponding star. The colors of the spectral lines correspond to the colors of the EW scatter points.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: The left panel shows the percentage of logDur in different bins, while the right panel shows the percentage of logAmp in different bins.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: FFD for stars of various spectral types. The red solid line represents the fitting results.
Paper: Magnetic Activity of TESS Objects Observed in the LAMOST Medium-resolution Spectral Survey
Authors: Tianhao Su, Li-yun Zhang, Prabhakar Misra, Xianming L. Han, Yinpeng Wang, Wenjie Li, Zhongzhong Zhu, Qingfeng Pi, Hongpeng Lu
Figure caption: Left panel: relationship between 〈EW〉 and σ EW. Right panel: relationship between 〈EW〉 and σ EW/〈EW〉. The red dots represent the median value of each bin.
Paper: A Geometric Approach to Estimate Background in Astronomical Images
Authors: Pushpak Pandey, Kanak Saha
Figure caption: Checking the contamination fraction in our generated images. From top to bottom, we increase the number of sources going from relatively uncrowded to very crowded. From left to right, we increase the mean background (λ), which goes from the low-count Poisson to the Gaussian limit of the Poisson distribution.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: 2D histogram comparing the fraction of events that are characterized (﹩{\pi }_{{\rm{E}}}\gt 2{\sigma }_{{\pi }_{{\rm{E}}}}﹩ and ﹩{t}_{{\rm{E}}}\gt 2{\sigma }_{{t}_{{\rm{E}}}}﹩) in baseline_v3.0_10yrs and baseline_v2.0_10yrs (baseline_v3.0_10yrs/baseline_v2.0_10yrs) for any given t E and π E. Bluer squares mean that more events were characterized in baseline_v3.0_10yrs, and redder squares mean that more were characterized in baseline_v2.0_10yrs. Gray squares mean that no events were characterized in either OpSim, in large part due to π E being intrinsically hard to measure with a single telescope for short-duration events (see Section 3.7). The bottom panel show the cadence of observations, where different colors represent different filters, as indicated in the legend, for the given OpSim in a 3.°5 × 3.°5 square centered on the R.A. and decl. indicated in the title of the left and right panels. The middle row shows the cadence of the OpSim in the numerator (baseline_v3.0_10yrs), and the bottom row shows the cadence of the OpSim in the denominator (baseline_v2.0_10yrs). The left panel is a representative bulge field, and the right panel is a representative disk field in a pencil beam. See Figure 2 for a realistic distribution of simulated events in π E − t E space. Since the baseline_v2.0_10yrs footprint included Galactic bulge and neglected the Galactic plane, the fraction of events characterized in the disk field event increased by ∼40%–50% in baseline_v3.0_10yrs and the fraction of events characterized in the Galactic bulge stayed about the same.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Same as Figure 7, but for each metric as a function of plane priority without pencil beams (pbf = pencil beams false). If the line is in the blue shaded region, this indicates that the OpSim performed better than baseline_v2.0_10yrs, and if it is in the red shaded region, it performed worse. As plane priority decreases, this means that areas of the Galaxy of lower priority are covered at a WFD-level cadence. The priorities are scientifically motivated regions of interest as defined in R. A. Street et al. (2023b). There is a peak around 0.6, but there is a significant drop when areas of priority 0.4 and lower are covered. This is because a finite number of visits are distributed over too large an area.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Plot of fraction of events detected (top), fraction of events with at least 10 points (middle), and fraction of events with σ tE/t E < 0.1 (bottom), relative to baseline_v2.0_10yrs as a function of the fraction included of the Galactic plane. These correspond to the results from the vary_gp family. The colors of the lines correspond to the timescale of the events, and the line style corresponds to the type of metric (dashed for Discovery, dotted for Npts, and dotted–dashed for Fisher). If the line is in the blue shaded region, this indicates that the OpSim performed better than baseline_v2.0_10yrs, and if it is in the red shaded region, it performed worse. In general, shorter-t  E  events are more affected by the change in cadence including random fluctuations. There is a significant decrease of microlensing characterization above gpfrac ≥ 0.55 since most microlensing events are in the Galactic bulge.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Same as Figure 8, but for each metric as a function of plane priority with pencil beams (pbt = pencil beams true). If the line is in the blue shaded region, this indicates that the OpSim performed better than baseline_v2.0_10yrs, and if it is in the red shaded region, it performed worse. Comparatively, the results are similar to those without pencil beams, with a significant drop when areas with priority 0.4 and below are included. Though a similar number of events are detected and characterized, the pencil beam fields were specifically chosen in R. A. Street et al. (2023b) to probe Galactic structure (and other scientific goals) throughout the Galactic plane.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Same as Figure 12, but comparing retro_baseline_v2.0_10yrs to baseline_v2.0_10yrs. Given the extremely sparse cadence in the Galactic bulge and plane in the retro baseline, we would characterize 60%–80% fewer microlensing events.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Same as Figure 5, but for the presto family, which explores triplets of observations within one night. The colors show the fractional improvement relative to baseline_v2.0_10yrs. Black vertical lines indicate separate OpSim families (summarized in Table 2), and black horizontal lines indicate separate metrics. Since most microlensing events do not vary significantly over the course of a night, when observations are taken over a less varied time period, this decreases detection and characterization efficiency.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Same as Figure 12, but comparing rolling_all_sky_ns2_rw0.9_v2.0_10yrs to baseline_v2.0_10yrs. This OpSim has the same footprint as baseline_v2.0_10yrs but with a rolling cadence. While this does not explicitly include the Galactic plane as part of the footprint with a rolling cadence, the fraction of events characterized in the bulge is ∼10% less than baseline_v2.0_10yrs.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Distribution of u 0, t E, and π E for simulated and characterized events. In blue are all of the simulated events, and in orange are those that are characterized (﹩{\pi }_{{\rm{E}}}\gt 2{\sigma }_{{\pi }_{{\rm{E}}}}﹩ and ﹩{t}_{{\rm{E}}}\gt 2{\sigma }_{{t}_{{\rm{E}}}}﹩) by the baseline_v3.0_10yrs OpSim in the bulge field R.A. = 263.°89, decl. = −27.°16.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Same as Figure 12, but comparing rolling_bulge_6_v2.0_10yrs to baseline_v2.0_10yrs. This has the same footprint as baseline_v2.0_10yrs but splits the bulge into six sections on which it alternates focus, as can be seen in the middle left panel. This leads to ∼20% fewer events being characterized in the Galactic bulge.
Paper: The Blue Horizontal-branch Stars from the LAMOST Survey: Atmospheric Parameters
Authors: Jie Ju, Bo Zhang, Wenyuan Cui, Zhenyan Huo, Chao Liu, Yang Huang, Jianrong Shi
Figure caption: The upper panel compares average BHB spectra with large and small ﹩\mathrm{log}g﹩ around t = 8000 K. The bottom panel shows the normalized residuals between these two average spectra, with the blue dots representing outliers exceeding three standard deviations. The black dashed lines represent the He absorption lines.
Paper: The Blue Horizontal-branch Stars from the LAMOST Survey: Atmospheric Parameters
Authors: Jie Ju, Bo Zhang, Wenyuan Cui, Zhenyan Huo, Chao Liu, Yang Huang, Jianrong Shi
Figure caption: The distribution of BHB stars in the Teff vs. ﹩\mathrm{log}g﹩ plane. The lines represent PARSEC, the theoretical isochrone tracks, with metallicity values of [Fe/H] = −2.5, −1.5, and −0.5, respectively. The tracks with ages of 1 Gyr are included in the figure.
Paper: The Blue Horizontal-branch Stars from the LAMOST Survey: Atmospheric Parameters
Authors: Jie Ju, Bo Zhang, Wenyuan Cui, Zhenyan Huo, Chao Liu, Yang Huang, Jianrong Shi
Figure caption: Posterior distributions of predicted Teff , ﹩\mathrm{log}g﹩, and [Fe/H]. The contours from the inside outward enclose the 68th, 95th, and 99th percentiles of the total probability in the three off-diagonal panels. The two vertical dashed lines in the three diagonal panels represent the lower and upper errors of the distribution at the 16th and 84th percentiles, respectively.
Paper: The Blue Horizontal-branch Stars from the LAMOST Survey: Atmospheric Parameters
Authors: Jie Ju, Bo Zhang, Wenyuan Cui, Zhenyan Huo, Chao Liu, Yang Huang, Jianrong Shi
Figure caption: Comparisons of predicted stellar labels (Teff, ﹩\mathrm{log}g﹩, [Fe/H]) of 12 BHB stars obtained from the SLAM to the prelabeled values as given by R. Wilhelm et al. (1999).
Paper: The Blue Horizontal-branch Stars from the LAMOST Survey: Atmospheric Parameters
Authors: Jie Ju, Bo Zhang, Wenyuan Cui, Zhenyan Huo, Chao Liu, Yang Huang, Jianrong Shi
Figure caption: The random errors of stellar parameters for duplicates as functions of S/N. The blue line represents the training flux only, and the red line represents the training flux and color index.
Paper: The Blue Horizontal-branch Stars from the LAMOST Survey: Atmospheric Parameters
Authors: Jie Ju, Bo Zhang, Wenyuan Cui, Zhenyan Huo, Chao Liu, Yang Huang, Jianrong Shi
Figure caption: The normalized spectrum of two stars. The black lines show the observed spectrum of the star. The red dashed line shows the theoretical spectra.
Paper: The Blue Horizontal-branch Stars from the LAMOST Survey: Atmospheric Parameters
Authors: Jie Ju, Bo Zhang, Wenyuan Cui, Zhenyan Huo, Chao Liu, Yang Huang, Jianrong Shi
Figure caption: Comparison of the stellar parameter between the SLAM estimates and the M. Xiang et al. (2022) results for the BHB stars.
Paper: Research on F10.7 Index Prediction Based on Factor Decomposition and Feature Enhancement
Authors: Shuainan Yan, Yanmei Cui, Bingxian Luo, Liqin Shi, Yanxia Cai
Figure caption: Correlation matrix depicting the relationships between the F10.7 index and three parameters. Panel (a) shows the correlation between FISXR and F10.7, (b) presents the relationship between new_Mag and F10.7, and (c) illustrates the association between XBF and F10.7. The vertical axis in the figures represents the F10.7 index, while the horizontal axis corresponds to the respective parameter values. The color intensity reflects the data density, with darker shades indicating regions of higher density.
Paper: Research on F10.7 Index Prediction Based on Factor Decomposition and Feature Enhancement
Authors: Shuainan Yan, Yanmei Cui, Bingxian Luo, Liqin Shi, Yanxia Cai
Figure caption: Plot of the F10.7 index before and after smoothing from 2021 to 2023. The original observed series is represented by the blue line, while the smoothed series is depicted in orange. The green scatter points indicate the jittered values. The orange line provides a clearer trend by reducing noise in the original data, allowing for an easier interpretation of long-term changes. The green scatter points highlight short-term variations in the observed data, providing insight into the instability inherent in the original measurements.
Paper: Research on F10.7 Index Prediction Based on Factor Decomposition and Feature Enhancement
Authors: Shuainan Yan, Yanmei Cui, Bingxian Luo, Liqin Shi, Yanxia Cai
Figure caption: Schematic of the proposed F10.7 prediction strategy. The left section of the figure illustrates the factor decomposition of the F10.7 index and the integration of additional features, including FISXR, new_Mag, and XBF, as key inputs to the model. The right section presents the iTransformer model framework, which consists of L Transformer blocks. The model outputs predicted smoothed and jitter values, which are then combined to generate the final predicted F10.7 value.
Paper: Research on F10.7 Index Prediction Based on Factor Decomposition and Feature Enhancement
Authors: Shuainan Yan, Yanmei Cui, Bingxian Luo, Liqin Shi, Yanxia Cai
Figure caption: Annual comparison of average error metrics between our model and those of other institutions from 2018 to 2023. Panels (a), (b), and (c) display the RMSE, MAE, and MAPE, respectively, over prediction horizons of 1–27 days.