adsabs/AstroCLIMB huggingface dataset:
Paper: The First Insight-HXMT Localization Catalog of Short-duration Gamma-Ray Bursts: The First Six Years
Authors: Shuo Xiao, Yan-Ting Zhang, Yue Wang, Yan-Qiu Zhang, Shao-Lin Xiong, Shuang-Nan Zhang, Shi-Jie Zheng, Jin-Peng Zhang, Peng Zhang, Cheng-Kui Li, Xiao-Bo Li, Shu-Xu Yi, Zhen Zhang, Bing Li, Hua Feng, Cong-Zhan Liu, Ming-Yu Ge, Xu-Fang Li, Zheng-Wei Li, Yu-Peng Xu, Xiang-Yang Wen, Jian-Chao Sun, Lian Tao, Qi-Bin Yi, Ce Cai, Yi Zhao, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, You-Li Tuo, Li-Ming Song, Fang-Jun Lu, Ti-Pei Li
Figure caption: Top and middle panels: the light curves of GRB 200415A recorded by Konus-Wind and ADC#1 (including detectors 1, 2, 3, 4, 5, and 6) of Insight-HXMT, the red shading shows the range of data discarded when calculating the cross-correlation function at the optimal time delay of 4.176 s. Bottom panel: scatterplot of cross-correlation function vs. time delay. Note that the time range for Konus-Wind discards is different for different delays.
Paper: The First Insight-HXMT Localization Catalog of Short-duration Gamma-Ray Bursts: The First Six Years
Authors: Shuo Xiao, Yan-Ting Zhang, Yue Wang, Yan-Qiu Zhang, Shao-Lin Xiong, Shuang-Nan Zhang, Shi-Jie Zheng, Jin-Peng Zhang, Peng Zhang, Cheng-Kui Li, Xiao-Bo Li, Shu-Xu Yi, Zhen Zhang, Bing Li, Hua Feng, Cong-Zhan Liu, Ming-Yu Ge, Xu-Fang Li, Zheng-Wei Li, Yu-Peng Xu, Xiang-Yang Wen, Jian-Chao Sun, Lian Tao, Qi-Bin Yi, Ce Cai, Yi Zhao, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, You-Li Tuo, Li-Ming Song, Fang-Jun Lu, Ti-Pei Li
Figure caption: Independence tests for different annuli. Therefore, as long as the data from both satellites used have not been overlapped at the same time, the localization results obtained are independent. The horizontal and vertical coordinates CRp and p represent p-values for the theoretical and calculated credible regions, respectively.
Paper: The First Insight-HXMT Localization Catalog of Short-duration Gamma-Ray Bursts: The First Six Years
Authors: Shuo Xiao, Yan-Ting Zhang, Yue Wang, Yan-Qiu Zhang, Shao-Lin Xiong, Shuang-Nan Zhang, Shi-Jie Zheng, Jin-Peng Zhang, Peng Zhang, Cheng-Kui Li, Xiao-Bo Li, Shu-Xu Yi, Zhen Zhang, Bing Li, Hua Feng, Cong-Zhan Liu, Ming-Yu Ge, Xu-Fang Li, Zheng-Wei Li, Yu-Peng Xu, Xiang-Yang Wen, Jian-Chao Sun, Lian Tao, Qi-Bin Yi, Ce Cai, Yi Zhao, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, You-Li Tuo, Li-Ming Song, Fang-Jun Lu, Ti-Pei Li
Figure caption: Localization map of GRB 200415A. The red annulus is obtained from HXMT-Konus (Wind) by discarding data saturation time ranges, which is consistent with the result obtained by IPN via Fermi (GBM), Odyssey (HEND), and Konus (Wind) (D. Svinkin et al. 2021).
Paper: The First Insight-HXMT Localization Catalog of Short-duration Gamma-Ray Bursts: The First Six Years
Authors: Shuo Xiao, Yan-Ting Zhang, Yue Wang, Yan-Qiu Zhang, Shao-Lin Xiong, Shuang-Nan Zhang, Shi-Jie Zheng, Jin-Peng Zhang, Peng Zhang, Cheng-Kui Li, Xiao-Bo Li, Shu-Xu Yi, Zhen Zhang, Bing Li, Hua Feng, Cong-Zhan Liu, Ming-Yu Ge, Xu-Fang Li, Zheng-Wei Li, Yu-Peng Xu, Xiang-Yang Wen, Jian-Chao Sun, Lian Tao, Qi-Bin Yi, Ce Cai, Yi Zhao, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, You-Li Tuo, Li-Ming Song, Fang-Jun Lu, Ti-Pei Li
Figure caption: Left panel: the black dots are the MCCF vs. time delay between KW and GBM observations of GRB 210605A, the red dotted line represents the most probable time delay for the original data. Right panel: the distribution of time delays obtained by MC.
Paper: The First Insight-HXMT Localization Catalog of Short-duration Gamma-Ray Bursts: The First Six Years
Authors: Shuo Xiao, Yan-Ting Zhang, Yue Wang, Yan-Qiu Zhang, Shao-Lin Xiong, Shuang-Nan Zhang, Shi-Jie Zheng, Jin-Peng Zhang, Peng Zhang, Cheng-Kui Li, Xiao-Bo Li, Shu-Xu Yi, Zhen Zhang, Bing Li, Hua Feng, Cong-Zhan Liu, Ming-Yu Ge, Xu-Fang Li, Zheng-Wei Li, Yu-Peng Xu, Xiang-Yang Wen, Jian-Chao Sun, Lian Tao, Qi-Bin Yi, Ce Cai, Yi Zhao, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, You-Li Tuo, Li-Ming Song, Fang-Jun Lu, Ti-Pei Li
Figure caption: The light curve of the extremely bright magnetar giant flare GRB 200415A observed by Insight-HXMT/HE. ADCs #1, #2 and #3 suffered data saturation in time ranges of (T0+0.011:T0+0.033 s), (T0+0.006:T0+0.032 s, T0+0.038:T0+0.052 s), and (T0+0.003:T0+0.031 s, T0+0.038:T0+0.052 s), respectively.
Paper: The First Insight-HXMT Localization Catalog of Short-duration Gamma-Ray Bursts: The First Six Years
Authors: Shuo Xiao, Yan-Ting Zhang, Yue Wang, Yan-Qiu Zhang, Shao-Lin Xiong, Shuang-Nan Zhang, Shi-Jie Zheng, Jin-Peng Zhang, Peng Zhang, Cheng-Kui Li, Xiao-Bo Li, Shu-Xu Yi, Zhen Zhang, Bing Li, Hua Feng, Cong-Zhan Liu, Ming-Yu Ge, Xu-Fang Li, Zheng-Wei Li, Yu-Peng Xu, Xiang-Yang Wen, Jian-Chao Sun, Lian Tao, Qi-Bin Yi, Ce Cai, Yi Zhao, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, You-Li Tuo, Li-Ming Song, Fang-Jun Lu, Ti-Pei Li
Figure caption: The effect of selecting different time-length backgrounds on time-delay (or localization) accuracy.
Paper: Atomic Transition Probabilities for UV and Optical Lines of Gd II 
Authors: G. T. Voith, E. A. Den Hartog, I. U. Roederer
Figure caption: Examples of calibration curves for the FTS (top) and ECH (bottom). The top panel shows redundant FTS sensitivity curves for spectrum 6 from the Ar I and Ar II BR method and from a W strip lamp. The bottom panel shows the sensitivity for spectrum 29 of the ECH as it changes in the low-dispersion direction. The rapidly changing sinc2(Δλ) behavior in the high-dispersion direction is not depicted.
Paper: Atomic Transition Probabilities for UV and Optical Lines of Gd II 
Authors: G. T. Voith, E. A. Den Hartog, I. U. Roederer
Figure caption: Comparison of observed and synthetic spectra around the Gd II line at 3395.12 Å for HD 222925 (top) and J2213−5137 (bottom). The small black squares mark the observed spectrum of each star. The solid red line marks the best-fit abundance, the shaded red band marks variations of ±0.3 dex from this best-fit abundance, and the black line marks a synthetic spectrum with no Gd.
Paper: Atomic Transition Probabilities for UV and Optical Lines of Gd II 
Authors: G. T. Voith, E. A. Den Hartog, I. U. Roederer
Figure caption: Logarithmic differences of experimental BFs measured in this study and those from DH06. The solid horizontal line at 0.0 indicates perfect agreement and error bars indicate the uncertainties of the two studies added in quadrature. It should be noted that these studies are not entirely independent. See the text for further discussion.
Paper: Atomic Transition Probabilities for UV and Optical Lines of Gd II 
Authors: G. T. Voith, E. A. Den Hartog, I. U. Roederer
Figure caption: Samples from several echelle spectra taken under different source conditions and normalized at the 3757.74 Å line of Gd II (12,318–38,922 cm−1). The variation of relative intensity of a line at 3758.31 Å originating from a different level of Gd II (3427–30,027 cm−1) and a Gd I line at 3757.94 Å (533–27,136 cm−1) is apparent.
Paper: Atomic Transition Probabilities for UV and Optical Lines of Gd II 
Authors: G. T. Voith, E. A. Den Hartog, I. U. Roederer
Figure caption: A-values from the theory of L. Radžiūtė et al. (2020) vs. the experimental A-values from this study. The solid diagonal line indicates perfect agreement, while the dashed lines indicate a factor of 2 disagreement.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Schematic for the derivation of the AIA PSF diffraction pattern. All images show an enlargement of the region around the PSF center. (a) Derive the 1D diffraction pattern of a grid of periodic slits. (b) Map the 1D diffraction pattern to two 2D images. (c) Convolve the two images to obtain the 2D diffraction pattern of a mesh. (d) Derive the diffraction pattern of the two entrance meshes of AIA. (e) Superimpose these diffraction patterns to obtain the complete diffraction pattern of the entrance mesh. (f) Derive the diffraction pattern of the focal plane mesh. (g) Convolve the diffraction pattern of the entrance mesh with the one from the focal plane mesh to obtain the complete AIA diffraction pattern.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: (a) Schematic of the AIA instrument. The active channel is selected in Telescopes 1, 3, and 4 by the focal plane filter located in the filter wheel and in Telescope 2 by the mechanical wavelength selector behind the entrance filter. Diffraction patterns are caused by two meshes supporting the entrance filter and by the one mesh supporting the focal plane filter. (b) Schematics of the arrangement of the meshes that support the entrance filter. (c) Dimensions of the meshes. Adapted from P. Grigis et al. (2012).
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: AIA PSF of the 193 Å channel as derived (a) by the AIA instrument team (P. Grigis et al. 2012) and (b) by B. Poduval et al. (2013). The PSF of the instrument team has a size of 4096 × 4096 pixels and consists of a PSF core, two diffraction patterns arising from two meshes that support the entrance filter, and one diffraction pattern from a mesh that supports the focal plane filter. The image only shows the diffraction patterns from the meshes supporting the entrance filter; the diffraction pattern of the mesh supporting the focal plane filter is very weak and cannot be seen here. The PSF derived by B. Poduval et al. (2013) has a size of 800 × 800 pixels, consists of the PSF core, the diffraction patterns, and a diffuse scattered light component.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Lunar-transit images taken by AIA in the 193 Å channel on 2013 March 11. (a) Original image. (b) Deconvolved image using the PSF of the AIA instrument team (P. Grigis et al. 2012). (c) Deconvolved image using the PSF of B. Poduval et al. (2013). Both deconvolved images still show a clear residual intensity profile in the lunar-occulted pixels.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Effect of the PSF deconvolution on the DEM reconstruction of a coronal hole. (a) Image of the coronal hole taken on 2016 October 30. The green contour outlines the region considered. (b) DEM reconstruction using the AIA 94, 131, 171, 193, 211, and 335 Å channels as input. The blue line shows the DEM reconstruction from the original AIA images. The yellow, green, and red lines show the DEM reconstruction from the PSF-deconvolved images using our new, the AIA team, and the Poduval PSFs, respectively. (c) Observed counts of the coronal hole in each AIA channel. For each channel, the orange line gives the median value, the box the 1σ range, and the extended error bars the 2σ range. (d) DEM reconstruction using only selected AIA channels. The blue line shows the reconstruction using the original AIA 171 and 193 Å channels. The orange line uses the deconvolved AIA 171 and 193 Å channels with our new PSF as input. The green, red, purple, and brown dashed lines, respectively, individually add the deconvolved 211, 131, 94, and 335 Å images to the deconvolved AIA 171 and 193 Å DEM reconstruction. The numbers above the peaks give the corresponding AIA counts that cause these peaks.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Evaluation of the new PSFs using the 2016 October 30 lunar eclipse images. Left: eclipse image. Right: intensity profile along the gray dashed line in the left image. The yellow lines are the intensities in the original AIA images, the red lines show the deconvolved intensities using our revised PSF, the green lines use the AIA team PSF, and the blue lines use the Poduval PSF. The rows from top to bottom show the results for the AIA 94, 131, 171, and 193 Å channels.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Evaluation of the new PSFs using 2011 September 8 images of an X 9.96 class flare. From left to right: original images, deconvolved images using our new PSFs, the AIA team PSFs, and the Poduval PSFs. From top to bottom: deconvolution results for the AIA 94, 131, 171, 193, and 211 Å channels.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Our new PSFs for all AIA channels. (a) Amount of diffracted and scattered light. The color-shaded areas show the probability distribution for the diffracted and scattered light. Each of the vertical stripes mark channels on the same AIA telescope. Left panels: fitted PSF weights for the 171, 131, and 335 Å channels. Right panels: amount of light that is diffracted and scattered farther than a given distance vs. the distance.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Continuation of Figure 19 for the AIA 211, 304, and 335 Å channels.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Effect of the PSF deconvolution on the AIA images of 2016 October 30. Left: original image. Center: deconvolved image using the revised PSFs. Right: percentage change from the original to the deconvolved image. From top to bottom: AIA 94, 131, 171, and 193 Å images.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Continuation of Figure 16 for the AIA 304 and 335 Å channels.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Continuation of Figure 14 for the AIA 193, 211, 94, and 304 Å channels.
Paper: Revised Point-spread Functions for the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory
Authors: Stefan J. Hofmeister, Daniel W. Savin, Michael Hahn
Figure caption: Continuation of Figure 20 for the AIA 211, 304, and 335 Å channels.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: Top left panel: reference image where the locations of the three slits used and the knots studied are indicated. Top right panel: the spectrum from Slit 1’s spectrum shows Knot 1’s [O III] λλ 4959,5007 emissions. Marked by the black arrow, Knot 1 has a radial velocity of −2190 km s−1, with a faint decelerated ablation tail extending ∼900 km s−1 from the knot. Bottom left panel: the spectrum for Slit 2. Knot 2, marked by the black arrow, has a radial velocity of −1950 km s−1 and an ablation tail that shows deceleration of ∼500 km s−1. Bottom right panel: the spectrum for Slit 3, showing [O III] emissions from Knots 3 and 4. Knot 3 has a radial velocity of −1800 km s−1 and a decelerated ablation tail extending ∼700 km s−1. Knot 4 has a radial velocity of +4800 km s−1 and has an ablation tail extending ∼500 km s−1 in radial velocity.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: Combined HST ACS/WFC 2022 November 27 F625W + F775W filter images of four northern regions exhibiting radially distorted ejecta morphology due to interaction with the reverse shock. The top panel shows the location of the four enlarged regions. Middle panels: east and west limb regions (A and D, respectively). Lower panels: neighboring regions (B and C) along Cas A’s northern shell boundary. North is up, east is to the left.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: Combined HST ACS/WFC 2004 March 4 F625W + F775W filter images of four southern regions exhibiting distorted ejecta morphologies following interaction with the reverse shock. The top panel shows the location of the four enlarged regions. Middle panels: SE and SW limb regions (A and D, respectively). Lower panels: neighboring parts (B and C) of the so-called parentheses feature near Cas A’s center. North is up, east is to the left.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: 2000 January WFC2 F675W, 2004 December ACS/WFC F6225W+F775W, 2010 November WFC3 F980M, and 2011 November WFC3 F980M images of Cas A’s southern limb showing the locations of P7, P8, and P9. Images are shown in the rest frame of the expanding ejecta. The appearance of new emission in the red boxes (6″ × 6″) is due to the proper motion of reverse shock relative to the ejecta. North is up, east is to the left.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: 2004 March ACS/WFC F850LP and 2011 November WFC3 F980M images of Cas A’s western limb showing the location of P12 in the sky frame. The appearance of new emission features (white) inside the red boxes between 2004 and 2011 (10″ × 10″) is due to the proper motion of reverse shock relative to the ejecta. North is up, east is to the left.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: 2004 March ACS/WFC F850LP and 2011 November WFC3 F980M images of Cas A’s southwestern limb showing the locations of P10 and P11. Images are shown in the rest frame of the expanding ejecta. The appearance of new emission features (white) inside the red boxes (6″ × 6″) are due to the proper motion of reverse shock relative to the ejecta. North is up, east is to the left.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: 2000 January WFC2 F675W, 2004 December ACS/WFC F6225W+F775W, and 2008 June WFC2 F675W of Cas A’s northwestern limb showing the locations of the P13, P14, and P15 regions. Images are shown in the rest frame of the expanding ejecta. The appearance of new emission in the red boxes (6″ × 6″) is due to the proper motion of reverse shock relative to the ejecta. North is up, east is to the left.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: 2004 December ACS/WFC F625W+F775W and November WFC3 F980M 2011 images of Cas A’s southeastern limb showing locations of P5 and P6 in the rest frame of the expanding ejecta. The appearance of new emission within the red boxes (6″ × 6″) is due to the proper motion of reverse shock relative to the ejecta. North is up, east is to the left.
Paper: Cassiopeia A’s Reverse Shock and Its Effects on the Expanding SN Ejecta 
Authors: Robert A. Fesen, Dan Milisavljevic, Daniel Patnaude, Roger A. Chevalier, John C. Raymond, McKinley Brumback, Kathryn E. Weil
Figure caption: Evolution of Cas A’s optical emission along its northwestern limb.
Paper: Dual-coding Contrastive Learning Based on the ConvNeXt and ViT Models for Morphological Classification of Galaxies in COSMOS-Web
Authors: Shiwei Zhu, Guanwen Fang, Chichun Zhou, Jie Song, Zesen Lin, Yao Dai, Xu Kong
Figure caption: Distributions of M (a), I (b), and D (c) for different types of massive galaxies. The top bars represent the median values of M, I, and D for different types of galaxies. The MIDs of the galaxies are gradually increasing from SPHs to IRRs.
Paper: Intelligent Forecasting for Solar Flares Using Magnetograms from SDO/SHARP, SDO/HMI, and ASO-S/FMG
Authors: Xuebao Li, Hongwei Ye, Yanfang Zheng, Ting Li, Jiaben Lin, Shunhuang Zhang, Pengchao Yan, Yongshang Lv, Noraisyah Mohamed Shah, Xuefeng Li, Xiaotian Wang, Yingbo Liu, Rui Wang, Jinfang Wei, Changtian Xiang, Honglei Jin
Figure caption: The magnetograms, corresponding heat maps, and regions of interest highlighted by the MViT model for two different samples with multiple ARs. Panels (a) and (d) display the C-class and M-class magnetograms, respectively, while panels (b) and (e) present the heat maps generated by the MViT model for the corresponding samples. Panel (c) is obtained by overlaying panels (a) and (b), and panel (f) follows a similar approach. AR 13435 produced an M-class flare at 12:48 UTC on 2023 September 21, while AR 13438 produced a C-class flare at 07:00 UTC on 2023 September 22.
Paper: Intelligent Forecasting for Solar Flares Using Magnetograms from SDO/SHARP, SDO/HMI, and ASO-S/FMG
Authors: Xuebao Li, Hongwei Ye, Yanfang Zheng, Ting Li, Jiaben Lin, Shunhuang Zhang, Pengchao Yan, Yongshang Lv, Noraisyah Mohamed Shah, Xuefeng Li, Xiaotian Wang, Yingbo Liu, Rui Wang, Jinfang Wei, Changtian Xiang, Honglei Jin
Figure caption: The magnetograms, corresponding heat maps, and regions of interest highlighted by the MViT model for the FMG, HMI_cropping, and SHARP data, respectively. Panels (a), (d), and (g) display the magnetograms of AR 13590 for the FMG, HMI_cropping, and SHARP data, respectively, while panels (b), (e), and (h) present the heat maps generated by the MViT model for the corresponding magnetograms. Panel (c) is obtained by overlaying panels (a) and (b), while panels (f) and (i) are generated using a similar method. AR 13590 produced an X-class flare on 2024 February 22 at 16:48 UT.
Paper: Intelligent Forecasting for Solar Flares Using Magnetograms from SDO/SHARP, SDO/HMI, and ASO-S/FMG
Authors: Xuebao Li, Hongwei Ye, Yanfang Zheng, Ting Li, Jiaben Lin, Shunhuang Zhang, Pengchao Yan, Yongshang Lv, Noraisyah Mohamed Shah, Xuefeng Li, Xiaotian Wang, Yingbo Liu, Rui Wang, Jinfang Wei, Changtian Xiang, Honglei Jin
Figure caption: The variation curves of TSS, recall, and FPR for the MViT model and NASA/CCMC with probability thresholds.
Paper: Intelligent Forecasting for Solar Flares Using Magnetograms from SDO/SHARP, SDO/HMI, and ASO-S/FMG
Authors: Xuebao Li, Hongwei Ye, Yanfang Zheng, Ting Li, Jiaben Lin, Shunhuang Zhang, Pengchao Yan, Yongshang Lv, Noraisyah Mohamed Shah, Xuefeng Li, Xiaotian Wang, Yingbo Liu, Rui Wang, Jinfang Wei, Changtian Xiang, Honglei Jin
Figure caption: Box plots of the performance results of the MViT model for FMG and HMI_cropping data.