adsabs/AstroCLIMB huggingface dataset:
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: Example light curves of different types of variables: linear, curved, periodic, burst, drop, and irregular from left to right. The LSP fitting and its period are shown in the upper panels. Here, the error bars are the uncertainties at individual epochs in the final light curve as calculated using Equation (1).
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: The fractional flux change between bright and faint epochs ΔW2 (y-axis) is plotted against the ratio of the standard deviation of the light curve and the mean flux uncertainty. Different classes of YSOs are plotted. The 1D distribution is shown at the top and right with a limited x-range for clear visibility. The 1D distribution of the “Uncertain” type is not shown due to low number statistics.
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: The p-value of the null hypothesis is plotted against the false-alarm probability of LSP. The vertical and horizontal lines indicate the limit to classify the YSO variability into different types.
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: Spectral index is plotted against mean W2 magnitude of our sources. The horizontal lines separate the YSOs into different classes. The W2 (mean) band magnitude distribution is shown at the top.
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: Flowchart illustrating the filtering process of YSOs from the initial sample to the final data set.
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: ΔW2 is plotted against SD/σ for different types of variables. Irregular variables are not shown due to their large sample size.
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: Left: The correlation between slope in color–magnitude diagram vs. spectral index (YSO class). Secular (linear, curved, and periodic), burst, drop, and irregular sources are also marked. The horizontal line denotes zero colors. Right: The slope of line fit of the color (W1 − W2) vs. W2 magnitude diagram. A negative slope indicates a redder-when-brighter (RWB) slope, while a positive slope indicates a bluer-when-brighter (BWB) trend.
Paper: Illuminating Youth: Decades of Mid-infrared Variability and Color Evolution of Young Stellar Objects
Authors: Sharma Neha, Saurabh Sharma
Figure caption: An example of BWB (left) and RWB (right) is shown. The magnitude is shifted in the first panel for better visibility.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Search for C9.6 flare on 2011 September 23 at 21:42:10.37 UTC recreated with GOES15 XRS-B with AIA-131 Å: example where canonical databases wrongly associate an AR to a flare in space and in time. Cluster 1 (orange) is associated with NOAA AR 11295 and HARP 856, and cluster 0 (blue) is associated with NOAA AR 11302 and HARP 892. Both SolarSoft and the SWPC report a flare that occurred within the ALEXIS integration region for cluster 1 (orange) for a C9.6-class flare but occurring at 21:43:00 UTC, which is incorrect. At the time reported by other databases (21:43:00 UTC), ALEXIS locates a flare of X-ray magnitude M2.9 at the opposite side of the Sun’s surface at the integration region for cluster 0 (blue). A precursor flare of magnitude C6.14 is detected by ALEXIS occurring at 21:34:42 UTC at region 1 (orange). Note that the duration of the flare the canonical databases mislabelled cannot be completely understood by relying on any method that only takes into account the information from the full solar disk, such as spectral line time series or XRS data. ML models will now include HARP 892 (cluster 0) and HARP 856 (cluster 1) into a positive class; previously, HARP 856 was wrongly placed in the positive class. The SWPC and SolarSoft are not specific or accurate for these entries. Both canonical entries are incorrect in time.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Search for C3.4 flare on 2014 January 5 at 18:17:20.29 UTC with GOES15 XRS-B with AIA-171 Å. ALEXIS locates a C6.97 flare at cluster 1 (orange) at 18:16:52 UTC related to NOAA AR 11944 and HARP 3563. Both canonical teams report the same flare related to cluster 1 (orange); SolarSoft returns a C3.4-class flare that is specific and accurate while the SWPC returns a C3.4 flare accurate but not specific. This example shows hidden emission associated with cluster 2 (green-NOAA AR 11946 and HARP 3580) that complicates the classical interpretation of the single-pixel XRS detector. The magnitude of the X-ray class for the flare occurring within cluster 1 will be overestimated because of the contribution to the X-ray signal that cluster 2 provides. Also, ALEXIS fails to pick up the flare at cluster 2 such that the HARP associated with this cluster will be incorrectly labeled when applying ML tasks. This is also an example where scientists might begin to question the influence of emission from one AR toward another.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Search for M2.8 flare on 2011 September 24 at 18:13:30.37 UTC with GOES15 XRS-B with AIA-131 Å. ALEXIS locates one M5.76 flare at 18:05:17 UTC within the integration box for cluster 0 (blue) and another M5.97 flare at 18:15:28 UTC within the integration box for cluster 1 (orange). SolarSoft and the SWPC located an M2.8 flare at 18:15:00 within cluster 0 (blue) and assigned them correctly to HARP 892 and NOAA AR 11302, but both teams report their flare incorrectly in time. This is an example of the duration of a flare being incorrect and the need for other metrics to label the magnitude of a flare. Without the emission from cluster 0, the magnitude of the flare emitting from cluster 1 (orange) would not be as strong. HARP 856 (NOAA 11295) for cluster 1 and HARP 892 for cluster 0 will be placed correctly into the positive class.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Search for C2.3 flare on 2013 May 1 at 18:52:30.32 UTC with GOES15 XRS-B with AIA-131 Å. There are two regions that are necessary in order to compose the single XRS signal. The duration of the flare as reported by other teams is incorrect; the XRS signal could not be reproduced without the C4.35 flare that occurs within the integration region for cluster 0 at 18:59:55 UTC. SolarSoft reported coordinates that are within the integration boundary of ALEXIS’s cluster 1 (orange) and thus accurate and specific for HARP 2691 and NOAA AR 11730. SolarSoft correctly identifies a flare occurring at 18:51:00 UTC, but note that the magnitude ALEXIS reports for this flare is C4.87. The signal of the integration region for cluster 0 has an increase to emission prior to the main emission for cluster 1. This raises the question of whether emission from one region may influence the release of energy at another region. Cluster 0 (blue) with HARP 2693 with NOAA AR 11731 was a previously unknown event and will now have the correct label for ML tasks.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Search for C7.0 flare on 2011 December 14 at 19:45:40.67 UTC with GOES15 XRS-B with AIA-304 Å. ALEXIS reports that this flare occurred at 19:46:15 within the integration region of cluster 1 (orange) represented by NOAA AR 11376 and HARP 1183. The emission of cluster 0 (blue) is necessary for the complete recreation of the single-pixel XRS flux. Cluster 0 (blue) could not be associated with any HARP or NOAA AR. This example shows how emission can be hidden and where ALEXIS fails to pick up flare peaks. The SolarSoft and SWPC metadata identify a flare in time but not in space; both the SWPC and SolarSoft are inaccurate and are not specific. HARP 1183 would be placed in the positive class while all other HARPs would be placed in the negative class. Note, this example also demonstrates how the duration of solar flares must be revisited, the need for a multipixel definition for when a solar flare occurred, and the increase in M-class flares number because of the XRS magnitude correction to new GOES instruments.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: SXI cleaning Hough transform, CCD bad readout example, NOAA center vs. ALEXIS. Left: postprocessed SXI image padded to a 512 × 512 image used in ALEXIS. The normalization of the image in this example has been exaggerated to demonstrate CCD bleeding due to the nature of how CCD potential wells behave during readout. Center: edge enhancements using the Canny filter with a σ = 3 from a Scikit image as a preprocessing step before applying the Hough transforms. Right: Hough transforms are used for identifying simple shapes in images with the help of an edge detector. The circular Hough transform was constrained to identify all pixels that together compose a border within a certain radius determined by the SXI’s resolution. On average, unprocessed SXI metadata report the solar center coordinates offset by 64″ (12 pixel space) when compared to the metadata from the ALEXIS processing. Validation of this method was done by reprojecting the SXI image onto AIA pixel space and comparing the location and coordinate conversion bright regions on the surface. The reprojection of images not processed by ALEXIS fail this test.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: ALEXIS catalog vs. SolarSoft vs. SWPC: bar plot showing how the flare subsample evaluated in this proof of concept compares to the entries found by ALEXIS. Each column in the plot is separated by flare magnitude bins (left: C-class flares; center: M-class flares; right: X-class flares). For each team (SWPC and SolarSoft), we show the census results in terms of accuracy (labeled Acc.) and specificity (labeled Spec.). From the bottom up: light pink follows entries in the SWPC that are correct, while yellow shows entries in SolarSoft that are correct. Next is the “gray zone,” where we show in light gray events that ALEXIS missed, and in the darker gray events ALEXIS found but that do not have a HARP. If the canonical teams have false positives, they are shown next in dark red. The “green” zone follows, with mint green showing events that the SWPC or SolarSoft incorrectly cataloged. The darker green on top shows events that are unique to ALEXIS, representing new flares that have never been described before.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Distribution of linear evaluation metrics. Each tile shows the linear agreement between the 1000 hr time ranges ALEXIS has optimized for. Top left: RMSE (Equation (3)). Bins have boundaries between 0.008 and 0.338 in 20 increments of 0.15. Top right: MSE (Equation (4)). Data have been binned at boundaries 7.537 × 10−5 and 0.103 in 20 increments of 0.005. Middle left: Pearson's correlation coefficient (Equation (2)). Data have been binned at boundaries 0.559 and 1.02 in 20 increments of 0.0219. Middle right: vector similarity scalar (Equation (6)). Data have been binned at boundaries 1.00 and 1.11 in 20 increments of 0.005. Bottom left: total energy (Equation (5)). Data have been binned at boundaries 0.758 and 1.34 in 20 increments of 0.029. Bottom right: distance from origin (Equation (7)). Data have been binned at boundaries 0.011 and 1.18 in 20 increments of 0.059.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Example of predicted signal vs. XRS signal for different RMSE bins. We show the fit of multiple or single contributions to the XRS signal. The XRS signal is in maroon, with the linear combination in gray, and each of the components on the linear combination in their respective colors (cluster 0 (blue), cluster 1 (orange), cluster 2 (green)). The x-axis is date-time with a tick mark every 5 minutes. The y-axis is normalized flux. Left: 0.0 ≤ RMSE < 0.05; center: 0.05 ≤ RMSE < 0.1; right: 0.1 ≤ RMSE: Bottom: enlarged example of RMSE distribution also seen in Figure 8.
Paper: Solar Cycle Variation of the Mass-loss Rate of Coronal Mass Ejections
Authors: Yijia Tang, 怡嘉 唐, Xiaojuan Zhang, 小娟 张, Hui Deng, 辉 邓, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Ying Mei, 盈 梅
Figure caption: Local and global wavelet spectra of monthly CME mass. From left to right these are all events, regular events, and specific events, and from top to bottom are the events over all time (from 1996 January to 2020 December), the events in solar cycle 23 (from 1996 January to 2008 December) and the events in solar cycle 24 (from 2009 January to 2020 December). The yellow color bars of the local wavelet power spectrum represent maximum power and the purple represents power. The region in the local wavelet spectra affected by the mother wavelet’s COI is shown by the crosshatched and shaded area, and the red dashed line in the global wavelet spectra corresponds to the 95% confidence level of red noise.
Paper: Solar Cycle Variation of the Mass-loss Rate of Coronal Mass Ejections
Authors: Yijia Tang, 怡嘉 唐, Xiaojuan Zhang, 小娟 张, Hui Deng, 辉 邓, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Ying Mei, 盈 梅
Figure caption: The monthly distribution of CME mass for all events, regular events, and specific events (top panel), the monthly distribution of the number of CMEs for all events, regular events, and specific events (middle panel) and the bottom panel shows the monthly distribution of the number of sunspots (SSN). The vertical dashed line divides solar cycle (SC) 23 and SC 24.
Paper: Solar Cycle Variation of the Mass-loss Rate of Coronal Mass Ejections
Authors: Yijia Tang, 怡嘉 唐, Xiaojuan Zhang, 小娟 张, Hui Deng, 辉 邓, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Ying Mei, 盈 梅
Figure caption: The monthly distribution of CME mass and flare flux at latitudes. Panels from top to bottom show all events, regular events, specific events, and flare flux.
Paper: Solar Cycle Variation of the Mass-loss Rate of Coronal Mass Ejections
Authors: Yijia Tang, 怡嘉 唐, Xiaojuan Zhang, 小娟 张, Hui Deng, 辉 邓, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Ying Mei, 盈 梅
Figure caption: The monthly distribution of high (blue line) and low (red line) latitude CME mass with the number of sunspots for all events, regular events, and specific events. The correlation (Cor.) coefficients of high (or low) latitude CME mass with the number of sunspots (SSN) are also given.
Paper: Solar Cycle Variation of the Mass-loss Rate of Coronal Mass Ejections
Authors: Yijia Tang, 怡嘉 唐, Xiaojuan Zhang, 小娟 张, Hui Deng, 辉 邓, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Ying Mei, 盈 梅
Figure caption: The monthly distribution of total X-ray peak flux for different-class flares. From top to bottom are class B, classes C and M, and class X, respectively. The vertical dashed line divides solar cycles 23 and 24.
Paper: Solar Cycle Variation of the Mass-loss Rate of Coronal Mass Ejections
Authors: Yijia Tang, 怡嘉 唐, Xiaojuan Zhang, 小娟 张, Hui Deng, 辉 邓, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Ying Mei, 盈 梅
Figure caption: Similar to Figure 5, but for the events at high latitudes.
Paper: Solar Cycle Variation of the Mass-loss Rate of Coronal Mass Ejections
Authors: Yijia Tang, 怡嘉 唐, Xiaojuan Zhang, 小娟 张, Hui Deng, 辉 邓, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Ying Mei, 盈 梅
Figure caption: Similar to Figure 5, but for the events at low latitudes.
Paper: X-Ray Spectral Variability of 13 TeV High-energy-peaked Blazars with XMM-Newton
Authors: P. U. Devanand, Alok C. Gupta, V. Jithesh, Paul J. Wiita, Archana Gupta
Figure caption: Ratio plots of PL model fits to eight observations having significant negative curvatures. The observation IDs, along with the source name, are displayed in each plot. The figures are rebinned for better pictorial representation.
Paper: X-Ray Spectral Variability of 13 TeV High-energy-peaked Blazars with XMM-Newton
Authors: P. U. Devanand, Alok C. Gupta, V. Jithesh, Paul J. Wiita, Archana Gupta
Figure caption: Top panels: relation between LP spectral parameters for all LP best-fit X-ray spectra. From the left: (a) curvature parameter β vs. photon index (at 1 keV) α; (b) α vs. spectral flux in the energy range of 2–10 keV, F2−10; (c) β vs. F2−10. Bottom panels: relation between LP spectral parameters for the 13 cases where we estimated peak energy in the studied energy range of 0.6–10 keV. From left: (d) curvature parameter βEPLP estimated from the eplogpar model fitting vs. synchrotron peak energy Ep in the rest frame; (e) isotropic peak luminosity vs. Ep. Data points of H1426+428 are represented as filled circles, while other data points are represented as filled squares.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Visualization of convex optimization. Left: title will include the evaluation metrics for the subset. The first row shows normalized flux vs. time, where light red represents the X-ray flux integrated across the whole solar surface while the vector created by the linear sum of discrete regions is shown in gray. Note the black squares and red diamonds that mark the peaks of the signal, which are necessary to define peaks, as described in Section 4.5. The second row shows normalized flux vs. time where the time series that compose the linear combination vector are traced in colors that follow the integration regions. Blue is reserved for cluster 0, orange for cluster 1, green for cluster 2, and purple for cluster 3. Note the diamonds color coded to the cluster regions and indicate the peaks in the time series used to define the peak time of a flare. The third row shows the 2 s XRS-B data (black solid line) vs. time where the flare metadata for SolarSoft (yellow) and the SWPC (red) are overlaid on top. Each team reports a flare peak time (solid vertical lines) and the duration of the flare (lighter-colored vertical span). Note the label on the third column shows the GOES flare class and peak time for each respective team. The fourth row shows the peak times defined by ALEXIS color coded by the cluster region that produced them, and the legend provides ALEXIS’s GOES X-ray class and peak time. Right: the title will include the original flare class the pipeline searches for and the central time stamp for the time range under analysis. The first row shows an image of the Sun at the wavelength that returned the best convex fit. The salmon-colored circle delineates the solar border, gray boxes show the HARP ARs available, and the colored boxes show the integration region of each cluster. Note the yellow and red triangles that show the location metadata as compiled by SolarSoft and the SWPC. If more than one flare is present in the canonical metadata for this time range, the triangle apex will be organized as follows: (upward) for the first flare in time, (downward) for the second flare in time, (left) third flare in time, (right) fourth flare in time. Below the main solar image, a zoomed-in region for each integration box is shown. The cluster the zoomed-in region belongs to is identified by the color of the border of the zoomed-in cutout. A colored dot representing the pixel returned by ALEXIS where the flare occurred is centered within the integration box. Specificity and accuracy: SolarSoft is accurate and specific for both entries. The SWPC is neither accurate nor specific in the first flare (orange) but is accurate and specific in the second flare (blue). See Section 5.2 for a discussion on accuracy and specificity.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: (A) Bar plot of GOES flares with or without locations from 2010 May to 2020 May: flares compiled from the Heliophysics Event Knowledgebase reported by GOES. They report if they have location metadata (purple) and if they do not have location metadata (gray). More than 50% of the C-class flares and above have no location metadata. (B) Differential analysis of the XRS signal: approximately 1 hr of data on 2014 January 7 at 22:31:30 UTC searching for a C7.4-class flare. Note that the XRS scale-corrected 2 s flux (maroon) will now push the magnitude of this flare into the M-class category; spline-fitted data (black); resampled data points at 3 minute cadence (blue scatter); time series of resampled points (blue line); magenta vertical lines show the local maxima. Note, SWPC and SolarSoft report one flare for this time range. ALEXIS returns two possible flares (the solid magenta vertical line is the first local maxima chronologically and the magenta dotted vertical line is the second local maxima). Upon completion of the pipeline, there are two flares that happened in this signal: the first is a C8.35 flare at 22:23:11 UTC with Helioprojective Cartesian (HPC) [–80”, –131”] associated with HARP 3563 close to the solar center and another M1.55 flare at 22:33:07 UTC with coordinates HPC [951”, 208”] close to the solar border and HARP 3587 (see Figure 5). (C) Distribution of all the local maxima found by differential analysis: SWPC (red), SolarSoft (yellow), and ALEXIS (purple). The differential technique recovers all but 372 events (4.3%). All of the missed events are recuperated when using the non-science-quality XRS data. ALEXIS identifies about 4 times the number of flares reported by other teams. This paper reports on a random sample of 1000 events from the center of the Venn diagram.