adsabs/AstroCLIMB huggingface dataset:
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: Similar to Figure 9, but for the Fe XV 284.16 Å line. Here, S CME and S AR are the initial areas at the height h 0.
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: Similar to Figure 2, but for a CME with slower acceleration.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The comparison of the effective temperatures derived from our method with the APOGEE DR17–calibrated values. The top-left panel shows the T eff comparison for dMs, while the top-right panel shows that for gMs. The bottom-left and bottom-right panels show the residuals’ distributions for dMs and gMs, respectively. The color scale and the contour lines indicate the number density of each region.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The comparison of the effective temperatures derived from our method with the literature values. The top-left panel shows the T eff comparison for dMs, while the top-right panel for gMs. The bottom-left and bottom-right panels show the residuals’ distributions for dMs and gMs, respectively. The color scale and the contour lines indicate the number density of each region.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: Samples of our fitting results with different spectral subtypes (from top to bottom: dM0, gM2, dM4, and gM6). Black and red lines are observed and model spectra, respectively. The designations and corresponding stellar parameters are listed, and the residuals between the model and observed spectra are shown at the bottom.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: Same as Figure 5, but for metallicity.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The distribution of T eff vs. ﹩\mathrm{log}g﹩ for common stars from APOGEE DR17. Stars are color coded in different metallicity groups.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: Same as Figure 5, but for surface gravity.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The initial guess values of T eff, ﹩\mathrm{log}g﹩, and [Fe/H]. Dots are color coded in different effective temperatures. Detailed information is listed in Table 1.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The distribution of T eff vs. ﹩\mathrm{log}g﹩ for common stars from the reference set. Stars are color coded in different metallicity groups.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The number of valid stellar parameters provided by 16 papers from the literature. See Table 2 for details.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: Same as Figure A1, but for surface gravity.
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: The geometric model of the CME structure. The CME is assumed to have a partial donut shape. (A) A self-similarly expanded CME geometry as seen from the polar side. The solid orange curve represents the CME structure (a partial donut shape) and the dashed orange curve depicts the same CME structure a while ago. The transition from the dashed orange shape to the solid orange shape shows the self-similar expansion of the CME structure. The dashed gray curves are the feet of the CME flux tube that we have neglected. The rectangle with gray stripes indicates the LOS projected CME area seen by the observer. (B) The lateral view of the CME geometry. The circle represents the circular cross section of the CME flux tube. The transition from the dashed circle to the solid circle describes the self-similar expansion. (C) The velocities at different parts of the CME structure (polar view). The orange and green curves indicate different shells within the CME structure. Details can be found in the text. (D) Similar to panel (C), but for the lateral view. (E) The lateral view of the CME structure in a spherical coordinate system. This figure is modified from Farmer (2005). (F) A cartoon illustration of the CME geometry in this work.
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: Synthetic profiles with different spectral resolutions and S/Ns at h 2 = 34.20 Mm, with a CME velocity of v 2 = 363.50 km s−1. S CME = 1%, S AR = 5%. Here, S CME and S AR are the initial areas at the height h 0. The left column shows the original profiles (black) and the single-Gaussian fitted components (blue); the line profiles were scaled with their maximum intensities normalized to unity. The right column shows the signals from the CME (residual profiles), after subtracting the single-Gaussian fitted components from the original profiles; the red line is the single-Gaussian fit to the residual profile. The corresponding S/N and ﹩\delta {\lambda }_{\mathrm{instr}}﹩ are denoted in the right column. The calculated ﹩\sigma ,{I}_{\max }﹩ and v CME are also indicated. Note that we normalized the spectral profiles before adding any noise, so the peak values of the synthetic profiles may sometimes exceed unity after the inclusion of noise (e.g., panels (C) and (G)).
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: Similar to Figure 5, but for a higher height h 9 = 55.30 Mm, with a larger CME velocity of v 9 = 930.56 km s−1. S CME = 1%, S AR = 5%. Here, S CME and S AR refer to the initial areas at the height h 0. Note that in panel (D), we did not perform a single-Gaussian fit for the residual profile, since it does not satisfy the 3σ criterion.
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: The line profiles of Fe XII 195.12 Å (left) and Fe XV 284.16 Å (right), averaged over the erupted loop region observed by Hinode/EIS. The black solid profiles with error bars are the observed profiles averaged over the small erupted region. The purple dashed profiles are the Gaussian fits to the blue-wing components caused by erupted plasma, the blue dashed profiles are the Gaussian fits to the primary components emitted from the background AR, and the orange dotted–dashed profiles are the double-Gaussian fits to the observed profiles.
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: The evolution of the CME height and velocity as a function of time. In the upper panel, the blue line represents v CME (the CME velocity from the best-fitted kinematic model) and the red line is v esc (the local escape velocity). In the lower panel, the black line is the CME height from the kinematic model. The vertical dashed line marks the time step where the CME is accelerated to the local escape velocity (v CME = v esc). The selected time steps used for further analysis are marked by the colored squares overlaid on the velocity and height profiles.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The recovered source-count function (as defined in Equation (9)) for the CPG μ  B (ε) construction (top left) and the NPTF ρ(f) construction (top right) in the realistic NuSTAR scenario. Each color represents a different random trial, with the 16% and 84% percentiles shown as dashed lines derived from the posterior. The true source-count function is shown in solid red. The gray fill shows the average percentile band, as a guide. The ρ(f) construction clearly recovers the incorrect source-count function, as the slope of the power-law is well outside all percentile bands. In comparison, the CPG construction is generally more accurate. The underestimation of sources in both methods is further discussed in the text. The same results, with the posterior conditioned to ω > 0.9, are shown in the bottom left and bottom right for CPG and NPTF, respectively. With this conditioning, the recovery of the total number of sources is drastically improved for the CPG.
Paper: Can We Detect Coronal Mass Ejections through Asymmetries of Sun-as-a-star Extreme-ultraviolet Spectral Line Profiles?
Authors: Zihao Yang, 子浩 杨, Hui Tian, 晖 田, Xianyong Bai, Yajie Chen, Yang Guo, Yingjie Zhu, 英杰 朱, Xin Cheng, Yuhang Gao, 宇航 高, Yu Xu, 昱 徐, Hechao Chen, Jiale Zhang
Figure caption: The procedures for synthesizing full disk-integrated line profiles by considering the effect of spectral resolution. The profiles correspond to the CME height of h 9 = 55.30 Mm. The initial area of the CME covers 1% of the solar disk, and ARs constitute 5% of the solar disk (including the initial CME area). (A) The black profile is the synthetic profile oversampled to a very small spectral pixel size, without any noise or degradation of the spectral resolution. The line profile is scaled with its maximum intensity normalized to unity. The red profile is the PSF-convolved profile with ﹩\delta {\lambda }_{\mathrm{instr}}﹩ of about 0.162 Å (FWHM). It can be seen that the profile is broadened due to the increased instrumental width (decreased spectral resolution). (B) The profile sampled with a spectral pixel size of about 0.162 Å/3.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The recovered source-count function for both the CPG μ  B (ε) construction and the NPTF ρ(f) construction in the ρ(f) scenario, described in the text. When all conditions for the construction of ρ(f) are met, both CPG and NPTF produce posteriors clustered around the injected population.
Paper: Radio-loud Quasars above Redshift 4: Very Long Baseline Interferometry (VLBI) Imaging of an Extended Sample
Authors: Máté Krezinger, Krisztina Perger, Krisztina Éva Gabányi, Sándor Frey, Leonid I. Gurvits, Zsolt Paragi, Tao An, Yingkang Zhang, Hongmin Cao, Tullia Sbarrato
Figure caption: EVN images at 1.7 and 5 GHz. The red cross indicates the Gaia optical position with its uncertainty, where available. In cases where the red crosses are too small, an additional large red “×” symbol marks the position. Its purpose is simply to guide the eye, and the size has no special meaning. The blue cross in the 1.7 GHz image denotes the 5 GHz VLBI position with the uncertainties of the 1.7 and 5 GHz positional difference for sources where the offset between the two VLBI radio positions is nonnegligible. The lowest contours are drawn at ±3 times the image noise. The positive contours increase by a factor of 2. The restoring beam is shown in the bottom left corner. Table 4 contains the image parameters.
Paper: Radio-loud Quasars above Redshift 4: Very Long Baseline Interferometry (VLBI) Imaging of an Extended Sample
Authors: Máté Krezinger, Krisztina Perger, Krisztina Éva Gabányi, Sándor Frey, Leonid I. Gurvits, Zsolt Paragi, Tao An, Yingkang Zhang, Hongmin Cao, Tullia Sbarrato
Figure caption: Radio continuum spectra of the 13 sources in our EVN sample. Black: total flux-density data collected from the literature. Blue: compact-component flux densities observed with high resolution in this project.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The variations of the loss value as a function of the degree of P  n . Top panel: the variation trends of the loss value for stellar parameters: T eff (red), ﹩\mathrm{log}g﹩ (orange), and [Fe/H] (blue) by changing the degree of the polynomial P  n . Bottom panel: the total loss value (weighted average of the three loss values above). To make the loss values of different stellar parameters comparable, each loss value is normalized to [0, 1].
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: A relational diagram of the terms defined and used in Section 4 and Appendix B, demonstrating the relationship between the terms graphically. (a) A single source located at  x  contributes s  B  counts to bin B as defined by the bin extents Ω B  (solid square). The number of counts is determined by the Poisson distribution P(s  B ∣ x ) as defined in the text. (b) Multiple sources located at { x   l } each contribute ﹩\{{s}_{i\to B}^{(j)}\}﹩ counts to bin B, creating a total of k  B  counts in the bin. (c) A Poisson process describes sources spatially distributed according to T( x ) (sketched by shaded region). Each source may contribute multiple photons to the bin, which are recorded as counts at locations { y   j }. (d) A single photon created by a source at  x  1 is converted to an expected number of counts using the following detector effects: the detector response (effective area and exposure time), κ( x  1), that is evaluated at the source location; the PSF distribution ϕ( y  2∣ x  1) evaluated at the location where the photon lands,  y  2, and conditioned on the source location; the detector efficiency, η( y  2), that is evaluated where the photon lands.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: Multiple simulated observations are formed into a mosaic for the final image. The color scale shows the total number of detected photons per bin. The gray dashed lines show the individual observations that comprise the mosaic. The axes are centered around an arbitrary sky location in units of arcminutes. The red inset shows the details of a few sources in this image. The color scale of the inset has been scaled by a square root to improve contrast. For one particular source within the inset, the white dotted lines are each perpendicular to the optical axes of the nearby observations, and show the direction along which the PSF lies for that observation. The simulation details are the same as Section 6.5, except that the density of sources is five times less, the average flux per source 600 times greater, and the bin size is five times smaller than the NuSTAR detector pixelization.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The recovered posterior in the number of point sources in the population, N, for both the novel CPG construction and the existing NPTF approach, for the three test scenarios considered in this work. Upright distributions are the posteriors for individual trials from the CPG construction. Inverted distributions are the posteriors recovered by NPTF. A clear bias away from the true number of sources, N true (red line), is observed from NPTF. We will describe the results shown here in detail in Section 6. For example, the extension of many posteriors to N ≫ N true is explained in Section 6.3.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The median recovered posterior for the novel natural coordinate system (top) and standard coordinate system (bottom), for multiple choices of priors on the number of sources (N, natural only), flux (F), and differential source-count function normalization (A, standard only). The posterior is shown for the fraction of flux assigned to the population model, as compared to a diffuse background model. In this scenario, only diffuse flux is present, and so these posteriors should be uniform, as diffuse emission is formally indistinguishable from a population of dim point sources. This is observed only for the natural coordinate system, with one exception discussed further in Section 5.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Left: the burst distribution of the whole burst sample. The best-fit log-Gaussian functions and corresponding mean values are shown by dotted lines. The blue, purple, black, and orange lines represent the duration of LE, ME, HE, and common, respectively. The red line is FRB 200428−Associated Burst. Right: the burst history of SGR J1935+2154 is shown in the top panel. Other captions of the top panel are the same as in Figure 5. The scatter of duration vs. their trigger time since 2020-04-28T00:00:00 is shown in the four lower panels. The gray dotted lines represent the time interval of no observation of Insight-HXMT (see also Table 1). The red star is FRB 200428−Associated Burst. Multipulse bursts are shown in red. The bursts with longer duration (larger than 350 ms, as marked by horizontal blue lines) are mostly found in the gray shaded regions.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Burst activity evolution of SGR J1935+2154 in 1-day time bins as seen with Insight-HXMT and Fermi/GBM (Lin et al. 2020b). The first burst in this activity phase was observed by Swift/BAT and Fermi/GBM around 2020-04-27T18:26:20.138. The start time of Insight-HXMT observation was about 13 hr later. There is no observation from 2020-04-29T12:02:36.000 UTC to 2020-04-30T06:58:23.000 UTC, resulting in incomplete monitoring of SGR J1935+2154 in these 3 days (purple dashed box; see also Table 1). The daily burst rate is the number of bursts divided by the effective exposure time when the source is monitored (i.e., the source is not blocked by Earth and the satellite is not in SAA). The blue and orange bars represent the burst rates of Insight-HXMT and Fermi/GBM, respectively. The red line is the trigger time of FRB 200428−Associated Burst.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Examples of Insight-HXMT-detected bursts of SGR J1935+2154. For each burst, light curves are shown for LE (1−10 keV; top panels), ME (10−30 keV; middle panels), and HE (28−250 keV; bottom panels). The background of each burst is shown by the blue dotted line. The events of LE data of burst #37 are lost owing to instrumental effects (e.g., bright Earth, bad events with higher grade). The HE data of burst #74 suffered from data saturation in the time interval marked as green shading. Burst #23 represents weak bursts in our sample with a trigger timescale of 0.01 s and trigger threshold of ∼5σ.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The distribution of waiting time for 21 time intervals (i.e., time difference between two successive bursts). The black dashed lines show the best-fit lognormal function with μ = 572 ± 82 s and σ = 0.44 ± 0.06 (the standard deviation in the logarithm scale). The distribution of the continuous observation time length is shown in the blue shaded regions (right vertical axis). The percentage of the continuous observation time length above 1000 s is 87%. The red line is FRB 200428−Associated Burst, whose trigger time is used to calculate waiting time for one time interval.