adsabs/AstroCLIMB huggingface dataset:
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: Dual-component “trend-disturbance” modeling and prediction framework for the FI. The workflow sequentially comprises three stages from left to right: scale decomposition, inference prediction, and result fusion. First, FI is decomposed into a smoothed component and a jitter component. Next, separate predictions are performed on the smoothed and jittered data. Finally, the predicted values of both components are fused to generate the final FI forecast. Each colored bar represents a single value at a specific time point. Green bars denote ﹩{\mathrm{FI}}_{\mathrm{jitter}}^{t}﹩, while yellow, red, blue, and purple bars represent ﹩{\mathrm{FI}}_{\mathrm{smooth}}^{t},F10.{7}^{t},{\mathrm{new\_Mag}}^{t}﹩, and XBFt, respectively; cyan and pink bars indicate ﹩{\hat{\mathrm{FI}}}_{\mathrm{jitter}}﹩ and ﹩{\hat{\mathrm{FI}}}_{\mathrm{smooth}}﹩.
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: Comparison between predicted and true values of ﹩\hat{{\rm{F}}}{{\rm{I}}}_{\mathrm{smooth}}﹩ and ﹩\hat{{\rm{F}}}{{\rm{I}}}_{\mathrm{jitter}}﹩ for Day 1 forecasts. (a) Predicted and true time series of ﹩\hat{{\rm{F}}}{{\rm{I}}}_{\mathrm{smooth}}﹩ (the vertical axis spans 0–600, and quantitative errors are reported in Table 6). (b) Predicted and true time series of ﹩\hat{{\rm{F}}}{{\rm{I}}}_{\mathrm{jitter}}﹩.
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: The fitted curve between FI and FImax. The scatter plot illustrates the distribution of the logarithmically transformed FI and FImax (logarithm base 10), while the red line represents the fitted curve. The gray dashed line indicates the diagonal reference line where FI equals FImax. The Pearson correlation coefficient and R2 value are 0.998 and 0.997, respectively.
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: Overall confusion matrix summarizing the classification performance of the FI threshold system across all years. The x-axis represents the flare classes as determined by the FI threshold system, while the y-axis represents the true flare classes.
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: The variation of the FI over the period from 1998 to 2024. FI is presented in a logarithmic scale, reflecting the intensity and frequency of flare activity. The blue box plots represent the distribution of FI values in a given year. The red dashed line represents the FI variations, while the purple line indicates the annual average sunspot number.
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: Comparison of short-term (1–3 days) M-class and X-class flare-forecasting performance across different models (2019–2024).
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: Example of data split based on the F10.7 index time series. The pink segment represents the training set, the yellow segment corresponds to the validation set, and the green segment indicates the test set.
Paper: Dual-stage Flare Prediction Using a Full-disk Flare Index: Trend-disturbance Decomposition and Hybrid Forecasting Model
Authors: Shuainan Yan, 帅楠 闫, Yanxia Cai, 燕霞 蔡, Bingxian Luo, 冰显 罗, Liqin Shi, 立勤 师, Yanmei Cui, 延美 崔
Figure caption: Forecasted daily maximum flare intensity (1–3 days) from 2024 May 1–15 across different models. Correct predictions are highlighted in green, and incorrect predictions (including missed alarms) are highlighted in red.
Paper: A Catalog of Filaments in the Central Molecular Zone
Authors: Richard G. Arendt, F. Yusef-Zadeh, I. Heywood
Figure caption: Histogram of filament widths. The red dashed line (at 2.25 pix = 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩475) indicates an adopted separation between likely real filaments and artificially narrow artifacts. The Gaussian smoothing applied to the data (σ1 = 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩75, Section 2) leads to a smoothed beam with σ = 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩23 in the filtered image.
Paper: A Catalog of Filaments in the Central Molecular Zone
Authors: Richard G. Arendt, F. Yusef-Zadeh, I. Heywood
Figure caption: (Left) Schematic curvature measurement at point B on a filament, bracketed by points A and C. The curvature, r, is a simple function of w, the half-length of segment ﹩\overline{AC}﹩, and z, the separation of B from the midpoint D of ﹩\overline{AC}﹩. See Equation (A1). (Right) Schematic curvature measurement for fitting a circular arc (dotted line) with radius r to a filament (connected dots) that has been rotated into a horizontal orientation. The algorithm actually fits for ρ ≡ 1/r since the relevant parameter range is then finite.
Paper: A Catalog of Filaments in the Central Molecular Zone
Authors: Richard G. Arendt, F. Yusef-Zadeh, I. Heywood
Figure caption: Map of filament spectral indices. Thermal emission with α ≳ −0.1 (yellow to red) appears mostly as short filaments with little organization at ∣b∣ < 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2. Supernova remnants with α ≈ −0.7 (green) appear as rounded clusters of curved filaments. The nonthermal radio filaments are more linear, oriented vertically, and generally have somewhat steeper spectral indices (blue).
Paper: A Catalog of Filaments in the Central Molecular Zone
Authors: Richard G. Arendt, F. Yusef-Zadeh, I. Heywood
Figure caption: Finder chart for catalog filaments having widths σg > 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩475. Each filament is labeled with its catalog number, but the numbers are very small to minimize confusion and the figure must be magnified to read them. The filaments and numbers are color coded by filament length (in arcseconds) to also help filament identification.
Paper: A Catalog of Filaments in the Central Molecular Zone
Authors: Richard G. Arendt, F. Yusef-Zadeh, I. Heywood
Figure caption: Map of filaments with selection criteria indicated by color. Gray indicates width σg < 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩475. Wider filaments are colored blue for lengths 33″ < L < 66″, green for 66″ < L < 132″, and red for 132″ < L.
Paper: A Catalog of Filaments in the Central Molecular Zone
Authors: Richard G. Arendt, F. Yusef-Zadeh, I. Heywood
Figure caption: Map of filament curvatures. Many of the straightest filaments (ρ ≈ 0) can be recognized as long nonthermal radio filaments here.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: The distribution plot of flares exhibiting QPP phenomena (M-type stars only). The left panel shows stacked plots for flare amplitude, duration, and flare energy, with green representing all flares and orange representing flares with QPP phenomena. For each parameter range corresponding to a bin, the proportion of flares with QPP phenomena relative to all flares in that bin is provided. In the right panel, a line plot of the proportion values with error for all bins is displayed.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: Six examples of flares exhibiting QPP phenomena, where the decay phase can be divided into two or more segments. Each of these flares has an energy exceeding 1035 erg, resulting in a rapid rise phase. The decay phase is split into two parts: the first segment shows no oscillations, while the second segment displays clear oscillatory behavior. In the figure, “contrast flux” represents the value obtained by subtracting the fitted background flux from the normalized flux.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: Relation between QPP period and other parameters. Panels (a)–(f) correspond to stellar effective temperature, stellar rotation period, flare amplitude, flare duration, flare energy, and flare ED, respectively.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: The distribution of flaring and nonflaring stars among FGKM spectral type stars. Blue represents nonflaring stars, and orange represents flaring stars. The percentage at the top of each bin for the flaring stars represents the proportion of flaring stars within the corresponding effective temperature range relative to the total number of stars in that temperature range.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: The distribution of stars with QPP flares. The top, middle, and bottom panels display the distribution of stars with QPP flares and the total number of flaring stars in each bin under different spectral types, effective temperature ranges, and rotation/orbital period ranges, respectively. In each panel, black represents all flaring stars, while red represents stars with QPP flares. For each bin, the red value indicates the proportion of stars with QPP flares relative to all stars in that bin. Using dual y-axes, this proportion is also plotted as a line chart to facilitate the observation of trends.
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: Panels (a)–(c): magnitude (from MQC) and redshift distributions for the 205 confirmed AGNs, 143 detected AGNs, and the final sample of 73 selected AGNs in the EGS field. Here, Bmag and Rmag denote the optical blue and red bands, respectively. The specific filters and central wavelengths vary by observational source. Panel (d): variability amplitude for the final catalog of 73 AGNs. Panels (e)–(f): for a subset of 17 AGNs (marked with stars), the distributions of (e) redshift versus absolute magnitude and (f) black hole mass versus bolometric luminosity are shown. In both panels (e) and (f), the blue and red points represent the two-dimensional parameter distribution from the larger AGN Physical Parameter Catalog (approximately 280,000 quasars) presented in S. Kozłowski (2017).
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: Schematic diagram of the overlapping region between ZTF and the EGS field. The left panel shows the coverage of ZTF’s three CCD-quadrants with the EGS field, along with the number of observations in the g, r, and i bands from 2018 March to 2024 December . The right panel illustrates the overlap between the blue CCD-quadrant (field 792 rcid 5) and the EGS field, with an overlapping area (marked by a solid red line) of approximately 10﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩2 × 37﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5. Yellow "x" symbols represent the 73 AGNs extracted in this study. Axes are in degrees.
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: The FWHM versus limiting magnitude for the g band (blue, left panel) and r band (orange, right panel). Vertical bars represent the limiting magnitude ranges for single-epoch data. In the g band, single-epoch medians are marked by squares and coadded values by stars. In the r band, single-epoch medians are marked by circles and coadded values by diamonds. Gray arrows connect single-epoch to coadded median points. Each data point is labeled with its corresponding sample bin (Bin 1–19).
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: The effects of bin placement and width on variability extraction for a sample light curve (ACSID 802), comparing the baseline scheme (gray vertical lines) against the test configurations (blue horizontal lines, A–K). The resulting light curves are shown as stars (test configurations), bold points (baseline coadded), and light points (traditional ZTF).
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: A small 5﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩3 × 3﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩7 cutout centered at α = 214﹩\mathop{.}\limits^{\unicode{x000b0}}﹩35, δ = 52﹩\mathop{.}\limits^{\unicode{x000b0}}﹩56 compares single-epoch (top) and coadded (bottom) images in two bands. All images are displayed using the same scale, contrast, and stretch.
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: Left: the relationship between the color index (g − r) and g-band magnitude for AGN ACSID 1280. Right: The distribution of the correlation coefficient r and significance level P for 73 AGNs. The shaded regions are colored blue (indicating a BWB trend), red (indicating an RWB trend), and gray (indicating no significant BWB or RWB trend, labeled as None).
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: Observation cadence of ZTF g-band (blue) and r-band (orange) exposures in field 792 rcid 5 from 2018 March to 2024 December. The gray vertical lines represent the range of each bin, the red numbers indicate the labels of each bin, and the black numbers represent the number of exposures in the g band and r band for each bin.
Paper: Optimizing Long-term Variability of Active Galactic Nucleus Light Curves. I. A Case Study with ZTF Observations in the EGS Field
Authors: Jiaqi Lin, 家琪 林, Zhen-Ya Zheng, 振亚 郑, Bin Ma, 斌 马, Lin Long, 琳 龙, Yangfan Xie, 扬帆 谢, Pu Lin, 浦 林, Ruqiu Lin, 如秋 林, Xiang Ji, 祥 吉
Figure caption: Schematic diagram of the data-processing workflow.
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: WISPR LW images showing the five blobs analyzed in this study. (a) Blob B1 appears in the lower-left corner of the field of view and remains visible for approximately 1.5 hr. (b) The faint blob B2 is visible in the upper-left corner for 2.5 hr. (c), (d) Blob B3 appears near the center of the field of view and persists for 5.8 hr. Blobs B4 and B5 are located in the lower half of the images, with durations of 3.4 and 3.3 hr, respectively. All blobs exhibit the typical SMFR characteristic of a central dark core surrounded by a brighter rim, sometimes incomplete. The SMFR morphology is particularly evident in B3 and B5. A streamer is also visible in the upper-left region of the field of view in panel (c).
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: WISPR LW (left) and LX (middle) images taken on 2025 December 25 at 03:15 UT reveal a notable contrast: the upper half appears relatively clearer in the LW image and darker in the LX image, suggesting the presence of a CH whose extrapolated boundaries intersect the WISPR FOV. These contrasting brightness patterns prompted a search for candidate CHs whose extended boundaries could account for the observed brightness depletion. A full-disk Atmospheric Imaging Assembly 193 Å image (right) taken on 2025 January 2 at 16:00 UT, when the CH was Earth facing, displays the identified candidate with its boundaries outlined in yellow dashed lines. HELIOS tool analysis confirmed that this CH was indeed the source of the brightness depletion observed in the WISPR images.
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: HELIOS 3D output for 2024 December 25, at 03:15 UT, presented in two perspectives. (a) Top-down view from solar north, showing the extrapolated CH boundaries and their intersection with the WISPR inner telescope’s FOV. (b) View from the perspective of a hypothetical observer positioned behind PSP, illustrating the relative positions of the spacecraft, the CH, and the WISPR FOV. The 3D reconstruction confirms that the candidate CH intersects the upper half of the WISPR images, with the greatest overlap—and thus the strongest brightness depletion—occurring near the upper-left corner of the image.
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: Extrapolated CH boundaries from the HELIOS 3D tool intersect the WISPR inner telescope’s FOV on 2025 December 25 at 03:15 UT, overlaid on the LX image (right panel). The CH’s extent aligns with the darker region in the LX images. For comparison, the actual LX image is shown on the left to facilitate direct visual inspection. The extrapolated lines are color coded by their angular separation from PSP.
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: The HELIOS 3D tool output for 2024 December 24 at 16:00 UT is shown in four different views. (a) View of the Sun and PSP from the perspective of a hypothetical observer located 0.25 au behind PSP (blue dot), which is at about 75° west of Earth. The gray region outlines the FOV of the WISPR inner telescope. The light-yellow surface shows the HCS, reconstructed in 3D from linear extrapolations (thin blue lines) of the PFSS solution between 2.5 and 30 R⊙. PFSS field lines are also visible extending from just above the solar surface to 2.5 R⊙. (b) Perspective from the location of the WISPR telescope, simulating the view of a hypothetical colocated observer. The HCS is prominently visible as it intersects the FOV (outlined in gray), revealing a complex folding structure near the center. PFSS extrapolation lines and the ADAPT magnetogram, mapped in 3D onto the solar surface, appear on the left, providing additional context of the solar environment. (c) Side view along PSP’s orbital plane, looking toward the Sun, illustrating the positions and orbits of PSP (blue), Earth (green), and the Sun at the center. The WISPR FOV is depicted as a gray pyramid. (d) Top-down view from solar north, illustrating the spatial relationship between the HCS and PSP’s orbital plane. The Sun is at the center, with PSP’s orbit and position shown in blue. The HCS intersects the WISPR FOV, and a segment of it runs nearly parallel to WISPR’s pointing vector—accounting for the absence of extrapolated lines at the FOV’s right edge, a feature more clearly seen in the lower portion of panel (b). A secondary conical HCS structure appears near 140°, to the left of the Sun–PSP line. In this view, the y-axis corresponds to the Sun–Earth line.
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: LOS geometry and intersections with HCS surfaces for blobs (a) B2 (2024 December 23, 16:15 UT), (b) B4 (2024 December 24, 22:00 UT), (c) B5 (2024 December 25, 03:15 UT), (d) B1 (2024 July 1, 04:45 UT), and (e) B3 (2024 December 24, 18:30 UT). The LOSs (black lines) intersect one to three HCS surfaces (magenta), with configurations ranging from simple (B2, B4, and B5) to complex folds (B1, B3). HCS structures intersecting the WISPR-I FOV are shown in gray scale, originating at 2.5 R⊙ (red) and extending to 30 R⊙ (blue), with shading indicating angular proximity to PSP. TF-estimated blob positions are marked (black dots).
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: Example of HCS lines reconstructed by the HELIOS 3D tool intersecting the WISPR inner telescope’s FOV on 2024 December 24 at 18:30 UT. The left panel displays the WISPR LW image showing the tracked blob B3 and the fitted ellipse (inset), indicating the center, major axis, and minor axis. Blob B3 displays a central darker region and a characteristic morphological “c” shape typical of most blobs. Coronal rays are visible in the top-left corner, along with a streamer. According to HELIOS, the streamer’s position at that time was at a Carrington longitude of 321° ± 3° and latitude of 20° ± 3°. The right panel shows the same image with the overplotted HCS lines. The color coding indicates their angular separation from PSP. The LOS connecting the observer to the ellipse intersects three HCS surfaces, with longitudinal separation angles of 77° ± 2°, 90° ± 2°, and 132° ± 1° relative to the Sun–PSP line.