adsabs/AstroCLIMB huggingface dataset:
Paper: Spectuner: A Framework for Automated Line Identification of Interstellar Molecules
Authors: Yisheng Qiu, Tianwei Zhang, Thomas Möller, Xue-Jian Jiang, Zihao Song, Huaxi Chen, Donghui Quan
Figure caption: Best-fitting results for SgrB2M-IRAM. Black lines represent the observed spectrum. Left and right panels show the results using the peak-matching and χ2 loss functions, respectively. The peak-matching loss function is described in Section 2.4.
Paper: Spectuner: A Framework for Automated Line Identification of Interstellar Molecules
Authors: Yisheng Qiu, Tianwei Zhang, Thomas Möller, Xue-Jian Jiang, Zihao Song, Huaxi Chen, Donghui Quan
Figure caption: Recall and precision of species identified in SgrB2M-IRAM. The red and blue bars represent the results using the peak-matching and χ2 loss functions, respectively. Definitions of recall and precision are provided in Section 4.1.
Paper: Spectuner: A Framework for Automated Line Identification of Interstellar Molecules
Authors: Yisheng Qiu, Tianwei Zhang, Thomas Möller, Xue-Jian Jiang, Zihao Song, Huaxi Chen, Donghui Quan
Figure caption: Computation time for our automated line identification algorithm using the peak-matching loss function.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: An example showing the CCD spatial distribution of residuals after applying the second-order two-dimensional polynomial correction. The panels, arranged from top to bottom, display the u, J0378, J0395, J0410, J0430, g, J0515, r, J0660, i, J0861, and z bands. The bands are labeled on the right, and a color bar is provided on top. From left to right, the first eight columns represent the selected eight tiles (SHORTS-STRIPE82_0087, SHORTS-STRIPE82_0088, SHORTS-STRIPE82_0090, SHORTS-STRIPE82_0092, SHORTS-STRIPE82_0094, SHORTS-STRIPE82_0098, SHORTS-STRIPE82_0100, and SHORTS-STRIPE82_0104), with the final column showing the combined residuals of these eight tiles. The tile number is indicated between the first-row panels and the color bar. To clearly show the spatial structure, the results for the u, J0378, J0395, J0410, J0430, g, and J0515 bands are compressed by two to three times.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Comparison of the zero-points for each of the SCR and XPSP standard stars for all 12 bands, as a function of star numbers (denoted as N) in each tile. The bands are marked in each panel. The green points show the difference of the zero-points. Their median values and standard deviations are estimated using Gaussian fitting with a running width of 15 stars and a running step of one star, and are indicated by the gray solid and red dashed curves, respectively. The median value of the standard deviations, for N ranging from 100 to 150, is labeled in each panel. The black dashed lines represent the zero-residual line. The distribution of zero-point differences is not strictly symmetric about zero at intermediate and/or large N, primarily due to the limited number of fields that the zero-points have in common. However, the decreasing trend of scatter with increasing N is clearly seen in all bands.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Examples of the spatial variations of the magnitude offsets between the XPSP standards and USS r-band photometry (the top-left panel), the magnitude offsets between the USS r-band magnitudes with aperture 6 and aperture 3 after aperture correction (the top-right panel), the normalized FWHM (the bottom-left panel), and ellipticity (the bottom-right panel). For the bottom-right panel, the points are displayed after removing the median of all points in the tile, and the median value is marked (in gray) in the top-right corner for each tile. The tile_ID is marked in each tile in black. The color bars are shown on top of the panels.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Examples of the medium-scale stellar flat field in the r band. The color bars are shown on top. Left panel: spatial variations of the magnitude offsets between the standard and USS photometry after FWHM- and large-scale stellar flat-field correction. The tile_ID is marked in each tile in black. Right panel: residuals after application of the second-order two-dimensional polynomial.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Examples of correlation plots of the magnitude offsets between the standards and the USS r-band photometry, as a function of the normalized FWHM. For each panel, the red plus signs denote the median values of the points, and the red lines denote the linear fitting result to the red pluses. The tile_ID (black), the correlation coefficient (green), and the slope (red) are marked in each panel. The gray number in each panel represents the magnitude offset in the aperture correction process.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Examples of the stellar flat field in the r band. Left panel: spatial variations of the magnitude offsets between the standards and USS r-band photometry after FWHM-dependent systematic error correction using a second-order two-dimensional polynomial (with six free parameters) fitting. The tile_ID is marked in each tile in black. Right panel: spatial variations of the magnitude offsets between the standards and USS r-band magnitude with APER_6. The color bars are shown on top.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Spatial variations of the second-order two-dimensional polynomial fitting residuals of the 42 tiles (left panel) and the results after 20 × 20 binning (right panel). The color bars are shown on top.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Correlation plots between the zero-point offsets predicted by the XPSP and the SCR standard stars for all bands. For each panel, the bands are marked in the top-left corner. The black dashed lines denote y = x in each panel; the gray dashed lines denote the zero level.
Paper: The S-PLUS Ultra-short Survey: Photometric Recalibration with the Best Star Database
Authors: Xiaolu Li, Kai Xiao, Yang Huang, Haibo Yuan, Yanke Tang, Timothy C. Beers, Bowen Huang, Mingyang Ma, Pedro K. Humire, Alvaro Alvarez-Candal, Federico Sestito, Ning Gai, Yongna Mao, Hongrui Gu, Zhenzhao Tao, Lin Yang, Shuai Xu, Rong Hu
Figure caption: Similar to Figure 14, but showing the results after applying both second-order two-dimensional polynomial and numerical stellar flat-field corrections.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 3, but for NVSS J141314-031227. Middle-left panel: radio map from VLASS centered at NVSS J141314-031227. Middle-right panel: W2 band infrared map of WISEA J141314.88-031227.5 (WISE counterpart to NVSS J141314-031227) from WISE. Right panel: SDSS optical map of the optical counterpart of WISEA J141314.88-031227.5.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 3, but for NVSS J160332+171158. Middle-left panel: radio map from VLASS centered at NVSS J160332+171158. Middle-right panel: W2 band infrared map of WISEA J160332.08+171155.3 (WISE counterpart to NVSS J160332+171158) from WISE. Right panel: SDSS optical map of the optical counterpart of WISEA J160332.08+171155.3.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 3, but for NVSS J141558+132024. Middle-left panel: radio map from VLASS centered at NVSS J141558+132024. Middle-right panel: W3 band infrared map of WISEA J141558.82+132023.7 from WISE. Right panel: SDSS optical map of the optical counterpart of NVSS J141558+132024.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J011322+251852. Middle-left panel: radio map from VLASS centered at NVSS J011322+251852. Middle-right panel: WISE W3 band infrared map centered at NVSS J011322+251852. Right panel: SDSS optical map centered at NVSS J011322+251852.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 3, but for NVSS J040845+001306. Middle-left panel: radio map from VLASS centered at NVSS J040845+001306. Middle-right panel: W1 band infrared map of WISEA J040845.31+001308.0. from WISE. Right panel: SDSS optical map of the optical counterpart of WISEA J040845.31+001308.0.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for 4C +26.07. Middle-left panel: radio map from VLASS centered at 4C +26.07. Middle-right panel: WISE W3 band infrared map centered at 4C +26.07. Right panel: SDSS optical map of the optical counterpart of 4C +26.07.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J004219+570836. Middle panel: radio map from VLASS centered at NVSS J004219+570836. Right panel: WISE W3 band infrared map centered at NVSS J004219+570836.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J055437+271126. Middle panel: radio map from VLASS centered at NVSS J055437+271126. Right panel: WISE W3 band infrared map centered at NVSS J055437+271126.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J033529+195621. Middle panel: radio map from VLASS centered at NVSS J033529+195621. Right panel: WISE W3 band infrared map centered at NVSS J033529+195621.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J094208+135152. Middle-left panel: radio map from VLASS centered at NVSS J094208+135152. Middle-right panel: W1 band infrared map centered at WISEA J094208.11+135155.0 (shown as a purple cross). The position of the background is shown as an orange cross. Right panel: SDSS optical map of the SDSS J094208.05+135154.9. The green square shows the position of the background radio source.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J104941+133255. Middle-left panel: radio map from VLASS centered at NVSS J104941+133255. Middle-right panel: WISE W2 band infrared map centered at NVSS J104941+133255. Right panel: SDSS optical map centered at NVSS J104941+133255. The bright orange point source below NVSS J104941+133255 is a star.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J080101-075121. Middle-left panel: radio map from VLASS centered at NVSS J080101-075121. Middle-right panel: WISE W2 band infrared map centered at NVSS J080101-075121. Right panel: SDSS optical map centered at NVSS J080101-075121.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J092351+281527. Middle-left panel: radio map from VLASS centered at NVSS J092351+281527. Middle-right panel: W2 band infrared map centered at NVSS J092351+281527. Right panel: SDSS optical map centered at NVSS J092351+281527.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J100755+405519. Middle-left panel: radio map from VLASS centered at NVSS J100755+405519. Middle-right panel: WISE W3 band infrared map centered at NVSS J100755+405519. Right panel: SDSS optical map of the optical counterpart of NVSS J100755+405519.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 3, but for NVSS J073755+264652. Middle-left panel: radio map from VLASS centered at NVSS J073755+264652. Middle-right panel: W3 band infrared map of WISEA J073755.33+264652.9 from WISE. Right panel: SDSS optical map of the optical counterpart of NVSS J073755+264652.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J095812+112643. Middle-left panel: radio map from VLASS centered at NVSS J095812+112643. Middle-right panel: WISE W3 band infrared map centered at NVSS J095812+112643. Right panel: SDSS optical map centered at NVSS J095812+112643.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 3, but for NVSS J095058+375758. Middle-left panel: radio map from VLASS centered at NVSS J095058+375758. Middle-right panel: W1 band infrared map of WISEA J095058.73+375758.3. from WISE. Right panel: SDSS optical map of the optical counterpart of WISEA J095058.73+375758.3.
Paper: The FAST H I 21 cm Absorption Blind Survey. II. Statistical Exploration for Associated and Intervening Systems
Authors: Wenkai Hu, Yougang Wang, Yichao Li, Wenxiu Yang, Yidong Xu, Fengquan Wu, Ue-Li Pen, Jie Wang, Yingjie Jing, Chen Xu, Qingze Chen, Zheng Zheng, Di Li, Ming Zhu, Xin Zhang, Xuelei Chen
Figure caption: Left panel: the same as Figure 2, but for NVSS J093150+254034. Middle panel: radio map from VLASS centered at NVSS J093150+254034. Right panel: WISE W2 band infrared map centered at NVSS J093150+254034.
Paper: PyEMILI: A New Generation Computer-aided Spectral Line Identifier
Authors: Zhijun Tu, Xuan Fang, Robert Williams, Jifeng Liu
Figure caption: Workflow chart of PyEMILI. The three main criteria of PyEMILI’s line identification are summarized separately in the three gray boxes in the bottom-right corner.
Paper: PyEMILI: A New Generation Computer-aided Spectral Line Identifier
Authors: Zhijun Tu, Xuan Fang, Robert Williams, Jifeng Liu
Figure caption: Top panel: optical spectrum of a Large Magellanic Cloud (LMC) [WC]-type star J0608. The red curve is the result of automatic continuum fitting by a function in the module SPEC of PyEMILI. During the continuum fitting, the length of the moving window is set to be 50 Å, while the percentile parameter is set to be 30%. Middle and bottom panels: examples showing automatic line searching in the spectrum (a) of J0608 by the PyEMILI module SPEC. The S/N threshold of emission lines is set to be 7. The continuum-subtracted spectrum is in black, and the spectral lines automatically found by PyEMILI are fitted using the Gaussian profiles in red and blue; the two colors are used alternately to distinguish the boundaries of two lines in proximity. The Gaussian profile in green in the middle-left and bottom panels is the line manually supplemented by the user through an interactive interface during line searching by the SPEC module. The middle-left panel demonstrates the fitting of P-Cygni profiles in the spectrum of J0608. The middle-right panel shows the profile fit of partially blended emission lines. The bottom panel demonstrates the SPEC fitting of the absorption lines in the spectrum. It should be mentioned here that the fitting of P-Cygni profiles is only a mathematically optimal solution.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Overview of the forward simulation of coronal loop kink oscillations with the stable measurement error, where a standard damping oscillation signal and its corresponding simulation signal are displayed as the black curve and plus signs on the top panel, the distributions of the fitted P and τ are presented in the middle and bottom panels, respectively.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Means and relative standard deviations of the fitted P (top), and relative deviations and standard deviations of the fitted τ (bottom) as functions of the model damping times, where the mean and relative standard deviation of the fitted p, or the relative deviation and relative standard deviation of the fitted τ are marked by the plus sign and rhombus, with their corresponding linear fitting results represented by three blue lines.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Means and relative standard deviations of the fitted P (top), and relative deviations and standard deviations of the fitted τ (bottom) as functions of the standard deviations of the measurement errors, where the mean and relative standard deviation of the fitted p, or the relative deviation and relative standard deviation of the fitted τ are marked by the plus sign and rhombus, with their corresponding linear fitting results represented by three blue lines.
Paper: The Error Estimation of Transverse Coronal Loop Oscillation Parameters Based on Least Chi-squares Fitting
Authors: Hongbo Li, Hengqiang Feng, Zhanjun Tian, Qiangwei Cai, Guoqing Zhao, Yan Zhao
Figure caption: Application examples of forward simulations on two observational loop kink oscillation cases, where the oscillation loops and their time-space slice are shown in the top panels, their fitting results are shown in the bottom panels. In the top-left panel, the position of the time-space slice is indicated by a white line labeled as “S.” The extracted oscillation signals are plotted as a series of white (black) plus signs on the top-right (bottom) panel, the fitting results of these signals are plotted as black curves in the bottom panels.