adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase
Authors: Pei Wang, Jian Li, Long Ji, Xian Hou, Erbil Gügercinoğlu, Di Li, Diego F. Torres, Yutong Chen, Jiarui Niu, Wei-Wei Zhu, Bing Zhang, En-Wei Liang, Li Zhang, Mingyu Ge, Zigao Dai, Lin Lin, Jinlin Han, Yi Feng, Chenhui Niu, Yongkun Zhang, Dejiang Zhou, Heng Xu, Chunfeng Zhang, Jinchen Jiang, Chenchen Miao, Mao Yuan, Weiyang Wang, Dengke Zhou, Jianhua Fang, Youling Yue, Yunsheng Wu, Yabiao Wang, Chengjie Wang, Zhenye Gan, Yuxi Li, Zhongyi Sun, Mingmin Chi, Junshuo Zhang, Jinhuang Cao, Wanjin Lu, Yidan Wang
Figure caption: The 2D kernel density estimation (KDE) of the pulses detected from SGR 1935+2154. Upper panel: the isotropic energy KDE (blue contours) assuming a distance of 6.6 kpc. Lower panel: the flux KDE (blue contours) and the average value for each observation session (black points).
Paper: X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase
Authors: Pei Wang, Jian Li, Long Ji, Xian Hou, Erbil Gügercinoğlu, Di Li, Diego F. Torres, Yutong Chen, Jiarui Niu, Wei-Wei Zhu, Bing Zhang, En-Wei Liang, Li Zhang, Mingyu Ge, Zigao Dai, Lin Lin, Jinlin Han, Yi Feng, Chenhui Niu, Yongkun Zhang, Dejiang Zhou, Heng Xu, Chunfeng Zhang, Jinchen Jiang, Chenchen Miao, Mao Yuan, Weiyang Wang, Dengke Zhou, Jianhua Fang, Youling Yue, Yunsheng Wu, Yabiao Wang, Chengjie Wang, Zhenye Gan, Yuxi Li, Zhongyi Sun, Mingmin Chi, Junshuo Zhang, Jinhuang Cao, Wanjin Lu, Yidan Wang
Figure caption: The distributions of the morphological fitting parameters α, β, and κ. In each of the lower-left plots of each panel, the points represent pulses with S/N > 10 from the set of 563 pulses detected. The error bars are calculated at the 68% confidence level. In each panel, the top plot is the histogram of the x-axis data, and the right plot is the histogram of the y-axis data. Panel (a) shows α vs β, a clear separation of the narrowband and broadband populations suggests β is a discriminating parameter between them. The two-component power-law distribution is separately fitted in a red solid line (panel (a2)), and the fitting residual is in the bottom (panel (a3)). Panel (b) shows κ vs. β, and panel (c) indicates κ vs. α.
Paper: X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase
Authors: Pei Wang, Jian Li, Long Ji, Xian Hou, Erbil Gügercinoğlu, Di Li, Diego F. Torres, Yutong Chen, Jiarui Niu, Wei-Wei Zhu, Bing Zhang, En-Wei Liang, Li Zhang, Mingyu Ge, Zigao Dai, Lin Lin, Jinlin Han, Yi Feng, Chenhui Niu, Yongkun Zhang, Dejiang Zhou, Heng Xu, Chunfeng Zhang, Jinchen Jiang, Chenchen Miao, Mao Yuan, Weiyang Wang, Dengke Zhou, Jianhua Fang, Youling Yue, Yunsheng Wu, Yabiao Wang, Chengjie Wang, Zhenye Gan, Yuxi Li, Zhongyi Sun, Mingmin Chi, Junshuo Zhang, Jinhuang Cao, Wanjin Lu, Yidan Wang
Figure caption: (a) Hardness-intensity diagram of SGR 1935+2154. The flux is in the 1.5–5 keV band. The red and pink data points are derived from NICER and Swift-XRT observations when SGR 1935+2154 shows radio pulsations, while the blue and black data points represent the rest of the NICER and Swift-XRT observations. The dashed red line represents the linear fitting of the observations when SGR 1935+2154 shows radio pulsations (red and pink data) points. (b) Cumulative χ 2 for observations when SGR 1935+2154 shows no radio pulsations against the linear fitting, showing a trend of deviation.
Paper: X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase
Authors: Pei Wang, Jian Li, Long Ji, Xian Hou, Erbil Gügercinoğlu, Di Li, Diego F. Torres, Yutong Chen, Jiarui Niu, Wei-Wei Zhu, Bing Zhang, En-Wei Liang, Li Zhang, Mingyu Ge, Zigao Dai, Lin Lin, Jinlin Han, Yi Feng, Chenhui Niu, Yongkun Zhang, Dejiang Zhou, Heng Xu, Chunfeng Zhang, Jinchen Jiang, Chenchen Miao, Mao Yuan, Weiyang Wang, Dengke Zhou, Jianhua Fang, Youling Yue, Yunsheng Wu, Yabiao Wang, Chengjie Wang, Zhenye Gan, Yuxi Li, Zhongyi Sun, Mingmin Chi, Junshuo Zhang, Jinhuang Cao, Wanjin Lu, Yidan Wang
Figure caption: The fluence and equivalent pulse-width distributions at 1.25 GHz for SGR 1935+2154. The dots indicate all of the 563 detected pulses, the red solid lines represent the equivalent brightness temperatures, and the horizontal blue dashed line is the simulated 90% detection completeness threshold. In the upper panel, an overall log-normal distribution is fitted as the gray line.
Paper: X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase
Authors: Pei Wang, Jian Li, Long Ji, Xian Hou, Erbil Gügercinoğlu, Di Li, Diego F. Torres, Yutong Chen, Jiarui Niu, Wei-Wei Zhu, Bing Zhang, En-Wei Liang, Li Zhang, Mingyu Ge, Zigao Dai, Lin Lin, Jinlin Han, Yi Feng, Chenhui Niu, Yongkun Zhang, Dejiang Zhou, Heng Xu, Chunfeng Zhang, Jinchen Jiang, Chenchen Miao, Mao Yuan, Weiyang Wang, Dengke Zhou, Jianhua Fang, Youling Yue, Yunsheng Wu, Yabiao Wang, Chengjie Wang, Zhenye Gan, Yuxi Li, Zhongyi Sun, Mingmin Chi, Junshuo Zhang, Jinhuang Cao, Wanjin Lu, Yidan Wang
Figure caption: Waiting-time–frequency distribution. We give the differential (green region) and cumulative (solid black line) distribution of waiting time, respectively. The solid red line represents an overall fit for the cumulative distribution of the pulse rate using a single threshold power-law function with an index of 1.96 ± 0.01, while the shaded region indicates fitting uncertainty.
Paper: X-Ray Hardening Preceding the Onset of SGR 1935+2154's Radio Pulsar Phase
Authors: Pei Wang, Jian Li, Long Ji, Xian Hou, Erbil Gügercinoğlu, Di Li, Diego F. Torres, Yutong Chen, Jiarui Niu, Wei-Wei Zhu, Bing Zhang, En-Wei Liang, Li Zhang, Mingyu Ge, Zigao Dai, Lin Lin, Jinlin Han, Yi Feng, Chenhui Niu, Yongkun Zhang, Dejiang Zhou, Heng Xu, Chunfeng Zhang, Jinchen Jiang, Chenchen Miao, Mao Yuan, Weiyang Wang, Dengke Zhou, Jianhua Fang, Youling Yue, Yunsheng Wu, Yabiao Wang, Chengjie Wang, Zhenye Gan, Yuxi Li, Zhongyi Sun, Mingmin Chi, Junshuo Zhang, Jinhuang Cao, Wanjin Lu, Yidan Wang
Figure caption: Lomb–Scargle periodograms of nulling periods for SGR 1935+2154. Nulling periods have been searched from 2 to 100 rotational periods, and no distinct concentration has been found in all of the active pulse phases.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: SED for the average source powering Lyα nebulae by stacking all 117 targets in this work. The observed data are from stacking of our Subaru/HSC g-band imaging (blue diamond), WISE imaging (orange squares), and VLASS S-band imaging (red circle). The black line denotes the best fit of CIGALE, together with the individual components: hot dust emission (red dashed line), cold dust emission (blue line), stellar emission (purple dashed line), and the radio emission from star formation (green dotted line). The best-fit galaxy stellar mass, SFR, and dust attenuation are annotated in the figure.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Upper: cutout images of MLAN44 in the WISE W1 (3.4 μm), W2 (4.6 μm), W3 (12 μm), and W4 (22 μm) bands, from left to right. The cutout size is ﹩2^{\prime} \times 2^{\prime} ﹩. Lower: the WISE IR color–color diagram of the matched and stacked sources in our sample. The blue-indexed 2D histogram denotes the distribution of sources with <0.3 mag errors in W1 (3.4 μ m), W2 (4.6 μ m), and W4 (22 μ m) in the all-sky release catalog with Galactic latitude b > 40°. Objects to the right of the dashed line are hot DOGs (P. R. M. Eisenhardt et al. 2012).
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Two Lyα nebulae with radio counterparts. The left panels present the smoothed continuum-subtracted Lyα line maps, and the right panels show the HSC g-band imaging. The cyan and white lines represent the 2σ and 5σ Lyα surface brightness contours. VLA 3 GHz radio observations from VLASS are overlaid as black contours of 5σ, 6σ, 7σ, 10σ, and 20σ, where σ = 0.15 mJy.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: The color–color distribution of the signal and contaminators in the training sample. The top panels are based on the data set without missing values (only 252 known high-redshift quasars), while the bottom panels are based on all the data in the data set (including 588 high-redshift quasars), where the missing values of high-redshift quasars are filled in by regression modeling; see Section 2.4 for detail. The tan square represents quasars with redshifts below 5, the black star stands for AFGK stars, the gray triangle is for MLT dwarfs, and the green dot represents the known high-redshift quasars. The orange dots and lines in each figure are the redshift trajectories of the known high-redshift quasars in the color space.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: The top panel presents the relation between photometric redshift and spectroscopic redshift as well as the distribution of the normalized Δz for the three regression algorithms (KNN, RF, CatBoost). The blue dashed line stands for Δz = ± 0.2, and the cyan dashed horizontal line represents Δz norm = ±0.1. The bottom panel presents the distribution of the difference between the photometric redshift and the spectroscopic redshift (Δz). The blue (red) dashed vertical line stands for Δz = ±0.2 (0.1). The numbers in the figure represent the fraction within the boundaries.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: Confusion matrix of the 11 class random forest classifier trained on FeatureSet-C for the test set. Each column in each row represents the predicted class counts for the corresponding true class. The percentages on the diagonal represent the precision of each class, and the shades of color represent the recall of each class. The precision of the high-redshift quasars is as high as 96.43%. The recall of the high-redshift quasars can achieve 91.53%, which means that approximately 10% of the high-redshift quasars are incorrectly predicted as other types.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: The distribution of the high-redshift quasars and the main contaminators, MLT dwarfs, in the 3D color space spanned by the z − W2, g − z, and r − grz features. It can be observed that the most important feature z − W2 from the random forest model is very effective to separate the high-redshift quasars from the contaminators in the 3D color space, while z − W2 is not effective in the traditional 2D color space.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: The distribution of g, r, W1, W2 magnitudes using various imputation methods. The red solid line represents the density distribution of the corresponding feature in the complete data set. The green, black, yellow, blue, and purple lines represent the density distributions of the respective features in the data sets imputed using the mean, LS limit, LR limit, RF, and MICE methods.
Paper: UVCANDELS: Catalogs of Photometric Redshifts and Galaxy Physical Properties
Authors: Vihang Mehta, Marc Rafelski, Ben Sunnquist, Harry I. Teplitz, Claudia Scarlata, Xin Wang, Adriano Fontana, Nimish P. Hathi, Kartheik G. Iyer, Anahita Alavi, James Colbert, Norman Grogin, Anton Koekemoer, Kalina V. Nedkova, Matthew Hayes, Laura Prichard, Brian Siana, Brent M. Smith, Rogier Windhorst, Teresa Ashcraft, Micaela Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Adam Broussard, Timothy Carleton, Nima Chartab, Alex Codoreanu, Seth Cohen, Christopher Conselice, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, Duilia De Mello, Mark Dickinson, Najmeh Emami, Henry Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven Finkelstein, Jonathan P. Gardner, Eric Gawiser, Timothy Gburek, Mauro Giavalisco, Andrea Grazian, Caryl Gronwall, Yicheng Guo, Pablo Arrabal Haro, Shoubaneh Hemmati, Justin Howell, Rolf A. Jansen, Zhiyuan Ji, Sugata Kaviraj, Keunho J. Kim, Peter Kurczynski, Ilin Lazar, Ray A. Lucas, John MacKenty, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Bahram Mobasher, Alexa M. Morales, Robert O'Connell, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Michael Rutkowski, Brant Robertson, Zahra Sattari, Emmaris Soto, Lei Sun, Sina Taamoli, Eros Vanzella, L. Y. Aaron Yung, Bonnabelle Zabelle
Figure caption: The difference between the galaxy stellar masses estimated from flexible (DENSE BASIS) and fixed (CIGALE) SFH approaches. The red curves show the running median (solid) and the 68% (1σ) percentile for the population. Even when fitting the same photometric data set with consistent assumptions, the inferred stellar masses are significantly impacted by the parameterization of the galaxy SFH during SED modeling.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: Footprint of the sky covered by the DR9 release of the Legacy Survey (A. Dey et al. 2019). The Galactic plane is traced by the red curve.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: The redshift distribution of the quasars in the training sample. The different colors represent the divided categories.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Distribution of spectral parameter values in different time intervals (histograms and corresponding normalized cumulative distribution (CDF) in the last panel of each row): curvature parameter (row (A)), photon index at 1 keV (B), 0.3–10 keV photon index (C), synchrotron SED peak position (D), and 0.3–10 GeV photon index ((E); 2 days of binned data).
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption:                         (a) Same as Figure 1 in the intervals listed in Table 4. Due to the strong correlation between the UVOT UVW–UVW2 band variabilities, only the plots from the shortest wavelength band are presented here (except for Interval 3). (b) The FACT-band light curve was available only for Period 2, and therefore, there are six panels in the corresponding plot. Since no FACT detections of the source with 3σ or higher occurred in Period 3, we had to add the sixth plot from the UVW1 observations. Note that the UVOT-band fluxes showed very strong cross correlations, and, therefore, only the UVW2-band light curve was generally plot in each period.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Fastest 0.3–10 keV IDVs detected at the 99.99% confidence level. The instances are arranged in order of increasing exposure.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Slower 0.3–10 keV variability from the densely sampled XRT observations.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: 0.3–10 keV IDV during densely sampled XRT observations, accompanied by flux doubling/halving.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: Probability for the high-redshift quasars vs. predicted redshifts for our catalog data. p quasar and z photo are provided by the “mag model.” The orange and cyan dots represent candidates predicted as the high-z class. The red and green dots represent known high-redshift quasars, with green dots indicating sources that are misclassified as other classes. The blue dots represent the known “mid-z” quasars in the training set that are incorrectly predicted as “high-z” class.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: The plot shows a step histogram of the probability of high-z candidates for the “mag model” (green area) and the “flux model” (red area). The sky blue area stands for the probability distribution of the candidates without missing values for the “flux model.” The step histogram is obtained by calculating the cumulative number of all data points from the largest probability bin (the leftmost bin) to the end of the current bin, with a width of 0.025 for each bin.
Paper: Machine Learning–based Search of High-redshift Quasars
Authors: Guangping Ye, 广平 叶, Huanian Zhang, 华年 张, Qingwen Wu, 庆文 吴
Figure caption: The MUSE spectra of these three “new” high-redshift quasars from our random forest model, with dashed vertical lines denoting the positions of the Lyα, N V, and C IV emission lines.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Correlation between the spectral parameters and MWL fluxes. The black, red, blue, purple, green, orange, brown, and gray points correspond to the data from Intervals 1, 2, 3, 4, 5, 6, 7, and 8, respectively.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Examples of extremely fast variability of the different spectral parameters. The top panel in each figure represents the unabsorbed F 0.3−10 keV flux, and the acronym “cgs” stands for erg cm−2 s−1.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Unabsorbed fluxes and spectral parameters plotted vs. time. (a) 0.3–2 keV flux; (b) 2–10 keV flux; (c) photon index at 1 keV (black points) and the 0.3–10 keV photon index (blue points); (d) curvature parameter; (e)–(f) position of the synchrotron SED peak (the upward and downward gray triangles indicate the lower and upper limits to the intrinsic position of the synchrotron SED peak, respectively; the lower limits are plotted separately for a better resolution). The Intervals presented in Section 3.1.1 are located between the vertical dashed lines.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: The spectra generated from each 100 s segment of ObsID 95330008, while the solid blue curve represents a log-parabolic model in panels (a)–d, (f), (h), and (j); it stands for a simple power law in panels (e), (g), and (i). In each case, the fit residuals are plotted in the bottom panel.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Examples of the different hysteresis patterns: rows (A) and (B) represent CW and CCW loops, respectively; (C): CCW-to-CW transition and/or vice versa. In each plot, the starting point is denoted by the symbol “1,” and the subsequent looping behavior can be traced by means of the red arrows.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: The WWZ (left column) and LSP (right column) plots in different spectral bands: panels (a) and (b) are based on the 1 day binned 0.3–10 keV and UVW2-band light curves, respectively; panel (c) is based on 1 week binned 0.3–300 GeV flux values.