adsabs/AstroCLIMB huggingface dataset:
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Curve distance between simulated (AWSoM) and measured (OMNI) plasma parameters for each CR. Except for a few outliers in one or two parameters, most distances are within the acceptable range, showing good agreement with OMNI observations.
Paper: Evaluating Time-series Augmentation Techniques for Deep Learning–Based Solar Flare Prediction
Authors: Peiyu Li, Omar Bahri, Soukaïna Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Comparing augmentation impact (recall, HSS, TSS, and Gini) using different methods under the MLSTM-FCN model.
Paper: Evaluating Time-series Augmentation Techniques for Deep Learning–Based Solar Flare Prediction
Authors: Peiyu Li, Omar Bahri, Soukaïna Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Comparing augmentation impact (recall, HSS, TSS, and Gini) using different methods under the FCN model.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Some examples of the different input magnetograms across different solar activity conditions. (a)–(b) CR 2102 is in the ramping-up phase of solar activity. (c)–(d) CR 2150 is near solar maximum. (e)–(f) CR 2212 is close to solar minimum. (g)–(h) CR 2271 is near the end of our data set, during a high solar activity phase.
Paper: Evaluating Time-series Augmentation Techniques for Deep Learning–Based Solar Flare Prediction
Authors: Peiyu Li, Omar Bahri, Soukaïna Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Comparing augmentation impact (recall, HSS, TSS, and Gini) using different methods under the ResNet model.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) Effects of varying the threshold values by 10% in the AIA images of the 193 Å channel. We can see that the trends do not change, but the identified region sizes differ. The y-axis represents the size of each region compared to the whole solar coronal disk. (b) Effects of varying the threshold values by 10% in the AWSoM images of the 193 Å channel. The overall trends do not change, but the identified region sizes can differ quite significantly.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: The workflow of the method. From the initial image, we create two binary images using two different thresholds, one for ARs, and one for CHs. Then, we run edge detection, and superpose the results on the initial image.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: An example of visual inspection of segmentation using an image taken of the Sun at 2014 July 4 08:00. The left panel was taken from Helioviewer with the identified ARs marked on the image. The right panel is from our AWSoM simulation at the same time, and the identified ARs are marked with green double outlines.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) The areas of identified ARs in the 171 Å channel images for AIA (blue solid), AWSoM (orange dashed), and MAS (green dashed–dotted). The gray curve denotes the f10.7 solar activity index. Near solar minimum, the area of ARs segmented on the AIA images seems to be overestimated. AWSoM generally follows the trend established on the AIA images, but overestimates the area near CR 120, while MAS overestimates it after solar maximum, near CR 2160. (b) Corresponding plot for the 171 Å channel for identified CH areas. The segmented CH areas are generally very small, even during solar minimum. (c) Corresponding plot for the 171 Å channel for identified QS areas.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) The areas of identified ARs in the 131 Å channel images for AIA (blue solid), AWSoM (orange dashed), and MAS (green dashed–dotted). The gray curve denotes the f10.7 solar activity index. Both models show very large areas for ARs during SC 25, but this channel gives good agreement between the models and AIA observations at other times. (b) Corresponding plot in the 131 Å channel for identified CH areas. AIA CH observations in this channel seem low near solar minimum. The models follow the same trends, but are different from the AIA observations. (c) Corresponding plot in the 131 Å channel for identified QS areas.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) The areas of identified ARs in the 193 Å channel images for AIA (blue solid), AWSoM (orange dashed), and MAS (green dashed–dotted). The gray curve denotes the f10.7 solar activity index. AR results in this channel show good agreement with the trend established by the solar activity index. Near solar maximum, AWSoM underestimates the area of ARs, while after solar maximum, near CR 2175, MAS overestimates it. (b) Corresponding plot in the 193 Å channel for identified CH areas. The CH trend mostly agrees with the AIA observations, although near solar minimum, both models seem to give smaller areas than AIA. (c) Corresponding plot for the 193 Å channel for identified QS areas.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: An example of two CHs observable on an AIA image “merging” into one larger CH in the AWSoM results. Both images are from 2011 March 9, 08:00. On the lower part of the disk, the AIA image clearly shows two distinct CH areas, which, in the AWSoM results, manifest as one larger CH with a somewhat different shape.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) The areas of identified ARs in the 335 Å channel images for AIA (blue solid), AWSoM (orange dashed), and MAS (green dashed–dotted). The gray curve denotes the f10.7 solar activity index. The visible trends for both models match up with the AIA observations. AWSoM somewhat underestimates the area of ARs during solar maximum, and MAS overestimates it near CR 2175. (b) Corresponding plot for the 335 Å channel for identified non-ARs.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) The areas of identified ARs in the 94 Å channel images for AIA (blue solid), AWSoM (orange dashed), and MAS (green dashed–dotted). The gray curve denotes the f10.7 solar activity index. AIA observations in this channel are heavily encumbered with noise, and do not give reasonable results. AWSoM and MAS results are also different. (b) Corresponding plot in the 94 Å channel for identified CH areas. Again, AIA gives unreasonable results due to heavy noise. AWSoM and MAS show similar trends, but the areas are different. (c) Corresponding plot in the 94 Å channel for identified QS areas.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) The areas of identified ARs in the 211 Å channel images for AIA (blue solid), AWSoM (orange dashed), and MAS (green dashed–dotted). The gray curve denotes the f10.7 solar activity index. Near the solar maximum of SC 24, MAS gives good results compared to AIA, while AWSoM underestimates the area of ARs. In SC 25, both models overestimate the area of ARs. (b) Corresponding plot in the 211 Å channel for identified CH areas. Near solar minimum, both models underestimate CH areas identified on the AIA images. (c) Corresponding plot in the 211 Å channel for identified QS areas.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) Differences between the observed (AIA) and simulated (AWSoM) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 171 Å channel. The gray curve denotes the f10.7 solar activity index. The largest differences are near CR 2120 and after CR 2250, where AWSoM overestimates the area of ARs. (b) Differences between the observed (AIA) and simulated (MAS) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 171 Å channel. The gray curve denotes the f10.7 solar activity index. After solar maximum, and during SC 25, MAS overestimates AR sizes.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Comparison of the calculated MAE values for each time period and each channel. The 193 Å channel provides the best results.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Histograms of all images combined on channel 171, for AWSoM, MAS, and AIA. The red vertical line represents the 25th percentile, the green line is the 50th percentile (or median), and the blue one is the 75th percentile.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) Differences between the observed (AIA) and simulated (AWSoM) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 193 Å channel. The gray curve denotes the f10.7 solar activity index. Although during SC 25, AWSoM is prone to overestimate ARs, it has very good agreement with observations. (b) Differences between the observed (AIA) and simulated (MAS) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 193 Å channel. The gray curve denotes the f10.7 solar activity index. AR results generally have low errors, but during SC 25, MAS overestimates the ARs.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) Differences between the observed (AIA) and simulated (AWSoM) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 131 Å channel. The gray curve denotes the f10.7 solar activity index. AWSoM overestimates ARs during SC 25. (b) Differences between the observed (AIA) and simulated (MAS) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 131 Å channel. The gray curve denotes the f10.7 solar activity index. In SC 25, AR areas are overestimated.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) Differences between the observed (AIA) and simulated (AWSoM) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 94 Å channel. The gray curve denotes the f10.7 solar activity index. The low SNR of the AIA channel heavily impairs our ability to draw meaningful conclusions. (b) Differences between the observed (AIA) and simulated (MAS) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 94 Å channel. The gray curve denotes the f10.7 solar activity index. The AIA channel is heavily affected by noise, which hinders the comparison.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) Differences between the observed (AIA) and simulated (AWSoM) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 211 Å channel. The gray curve denotes the f10.7 solar activity index. AWSoM underestimates ARs during solar maximum, but overestimates them during SC 25. (b) Differences between the observed (AIA) and simulated (MAS) AR (orange), CH (blue dashed), and QS (green dashed–dotted) areas in the 211 Å channel. The gray curve denotes the f10.7 solar activity index. MAS overestimates the ARs during SC 25.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: (a) Differences between the observed (AIA) and simulated (AWSoM) AR (orange) areas in the 335 Å channel. The gray curve denotes the f10.7 solar activity index. The period after CR 2250 shows overestimation then underestimation of AR sizes. (b) Differences between the observed (AIA) and simulated (MAS) AR (orange) areas in the 335 Å channel. The gray curve denotes the f10.7 solar activity index. There are periods with higher error near CR 2120 and 2175 and after CR 2260.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Histograms of all images combined on channel 193, for AWSoM, MAS, and AIA. The red vertical line represents the 25th percentile, the green line is the 50th percentile (or median), and the blue one is the 75th percentile.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Histograms of all images combined on channel 335, for AWSoM, MAS, and AIA. The red vertical line represents the 25th percentile, the green line is the 50th percentile (or median), and the blue one is the 75th percentile.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Histograms of all images combined on channel 211, for AWSoM, MAS, and AIA. The red vertical line represents the 25th percentile, the green line is the 50th percentile (or median), and the blue one is the 75th percentile.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Histograms of all images combined on channel 131, for AWSoM, MAS, and AIA. The red vertical line represents the 25th percentile, the green line is the 50th percentile (or median), and the blue one is the 75th percentile.
Paper: Validation of Long-term Solar Coronal Modeling Using FORWARD
Authors: Gergely Koban, Judit Szente, Bart van der Holst, Gabor Toth, Enrico Landi
Figure caption: Histograms of all images combined on channel 94, for AWSoM, MAS, and AIA. The red vertical line represents the 25th percentile, the green line is the 50th percentile (or median), and the blue one is the 75th percentile.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Top: absolute magnitude distribution 1319 frames of 406 detected comets in the W1 and W2 bands as a function of heliocentric distance (rH), shown separately for preperihelion (panel (a)) and postperihelion (panel (b)) detections. The dashed curves indicate limiting magnitude trend lines based on the W1-band (16.3 mag, black) and W2-band (14.8 mag, gray) detection thresholds (Figure 10), assuming the typical WISE/NEOWISE observing geometry (∼90° solar elongation). Bottom: linear brightness slopes (units of mag au–1) computed from pairs of consecutive detections in the W1 or W2 bands, where two consecutive epochs in the same band occurred either both pre- or both postperihelion. Panels (c) and (d) show the slope distributions as a function of rH. Horizontal bars indicate the rH separation between the paired detections. Comets are color coded by dynamical group.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Magnitude distributions across the four WISE/NEOWISE bands. Hatched histograms represent fixed-aperture photometry (Section 2.5) for detected comets with S/N > 4. Overlaid in purple are the magnitudes of comets submitted to the MPC under observatory code C51.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Distributions of the antisolar vector r⊙ (right) and negative velocity vector −v (left) for 1335 queryable comets (Section 2.1) as a function of heliocentric distance (rH). Daily variations are shown as golden background strands. Colored circles denote the vector orientations and rH values for 966 epochs of 485 detected comets, with SPCs and LPCs color coded separately. Vertical dashed lines indicate the 1.3 au perihelion threshold for NECs.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Brightness evolution of comets as a function of heliocentric distance, grouped by band and dynamical class. The top two panels and the bottom two panels correspond to LPCs and SPCs, respectively. Only comets observed more than twice were included. Absolute magnitudes (Equation (1)) are connected by lines. JFC 29P/Schwassmann–Wachmann was excluded due to limited rH coverage. The dashed curves indicate the limiting magnitude trend lines based on the W1- and W2-band detection thresholds (16.7 mag and 16.0 mag, respectively; Figure 10), assuming typical WISE/NEOWISE observing geometry (∼90° solar elongation).
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Activity distribution across 966 epochs for 484 detected comets (Table B1) as a function of true anomaly (ν). The top, middle, and bottom rows correspond to all (both long- and short-period) comets, LPCs, and SPCs, respectively, with each group divided into active (left) and inactive (right) subsets. Color gradients indicate S/N-based quality grades, with darker shades denoting higher confidence (grade A = darkest). Gaussian fits are overlaid for approximately symmetric distributions to highlight peak locations. The background pulses seen in the SPCs (bottom row) are artifacts of binning and do not reflect physical features.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Orbital element distribution of 484 detected comets. Solid and dotted black lines indicate TJ = 3 boundaries; gray lines show TJ = 2 boundaries for inclinations of 0°  and 12﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 (median i of SPCs). Vertical dashed lines mark the perihelion threshold (q = 1.3 au) separating NECs from others. Acronyms for each comet group are defined in the main text.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Comparison of detected (pink, S/N > 4) and MPC-submitted (black) comet detections as a function of perihelion distance (q, panel (a)) and heliocentric distance (rH, panel (b)). Panel (c) shows their sky distribution in R.A. and decl. “E” and “G” indicate the ecliptic and Galactic planes, respectively; the Galactic center is marked by a green diamond at R.A. = 266﹩\mathop{.}\limits^{\unicode{x000b0}}﹩405, decl. = −28﹩\mathop{.}\limits^{\unicode{x000b0}}﹩936.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Distribution of primary PAs for 695 frames of 255 comets classified as Y-A (active with S/N > 10) across the W1–W4 bands, plotted against orbital inclination (i). The PA measurements follow the method described in Section 2.4. The dynamical group symbols match those in Figure 14.
Paper: COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets
Authors: Yuna G. Kwon, Dar W. Dahlen, Joseph R. Masiero, James M. Bauer, Yanga R. Fernández, Adeline Gicquel, Yoonyoung Kim, Jana Pittichová, Frank Masci, Roc M. Cutri, Amy K. Mainzer
Figure caption: Comparison of magnitudes derived using photutils.aperture (as applied in this study) with those from the WISE Single-Exposure Source Catalogs for 1000 randomly selected asteroids spanning a wide brightness range during the WISE Cryo phase.
Paper: Metallicities of 20 Million Giant Stars Based on Gaia XP Spectra
Authors: Lin Yang, 琳 杨, Haibo Yuan, 海波 苑, Bowen Huang, 博闻 黄, Ruoyi Zhang, 若羿 张, Timothy C. Beers, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Yang Huang, 样 黄, Maosheng Xiang, 茂盛 向, Meng Zhang, 萌 张, Jinming Zhang, 津铭 张
Figure caption: Comparison of [Fe/H] for common stars between this work and B. Huang et al. (B. Huang et al. 2025; left panels) as well as A. Viswanathan et al. (2024; right panels). The left panels are color coded by number density. The first row presents our estimates, as a function of [Fe/H], from the two literature sources. The black solid line is the one-to-one line. The lower three rows display Δ[Fe/H] as a function of [Fe/H] from the two sources, G magnitude, and intrinsic BP − RP color, respectively. The black solid lines represent the mean deviation and the 1σ uncertainty of the residuals.