adsabs/AstroCLIMB huggingface dataset:
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of N ≥ 3 systems with one or more detected outer planets, ordered by the period of the first outer planet. All known outer planets under our definition are Jupiters, although this is not a definitional requirement. Five systems do not have any detected inner planets. The outer planets are systematically wider spaced in period ratio than the inner planets.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of multiplanet systems (including two-planet systems) that include a USP with P < 1 day. The USPs have a variable degree of dynamical detachedness from the other (usually peas-in-a-pod) planets in their systems. Kepler-42 is the only system with additional planets within P < 2 days.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Scatter plot of mass ratios vs. inner-planet masses for adjacent pairs of planets in two-planet (purple), three-planet (green), and higher-multiplicity systems (orange). Each dot represents one pair of planets, for N − 1 dots per system. The two-planet systems include more systems with large masses, as is evident from the abundance of purple points at high Mi values.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: The same as Figure 6 but for period ratios vs. inner-planet periods. The two-planet systems show more systems with large period ratios, as is evident from the abundance of purple points near the top of the plot. Meanwhile, the higher-multiplicity systems show more similarity to one another in both plots.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of gapped peas-in-a-pod systems with N ≥ 3 inner planets, divided by gap location and ordered by a location-specific measure of “gap period.” This figure includes all systems in Figure 9 that do not have Jupiters among their inner planets, but is extended by systems with only three inner planets (also restricted to non-Jupiters).
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: (a) Processed Stokes I data for beam M08, mapping the blazar J0854+2006 during observations conducted in 2021. The feature near the bottom of the map is attributed to a nearby secondary source, J0854+1959, which is close enough to contribute to the observed data. (b) Results of the log-normal combined with Gaussian fitting applied to the Stokes I data. (c) Residual map showing the differences between the Stokes I data and the fitting results. White solid lines indicate contour levels at 2%, 10%, 30%, 50%, 70%, and 90% of the peak flux.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: Stokes I mapping of J0854+2006 for the 19 beams near 1420 MHz. To compare with the simulated beam structures (as shown in Figure 7), the mapping data has been mirror-symmetrized. The feature near the source of each map is attributed to a nearby secondary source, J0854+1959. White solid lines indicate contour levels at 1%, 2%, 10%, 30%, 50%, 70%, and 90% of the peak flux.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: (a) Processed Stokes I data for the central beam, mapping the blazar J0854+2006 during observations conducted in 2021. The feature near the bottom of the map is attributed to a nearby secondary source, J0854+1959, which is close enough to contribute to the observed data. (b) Results of Gaussian fitting applied to the Stokes I data. (c) Residual map showing the differences between the Stokes I data and the Gaussian fitting results. White solid lines indicate contour levels at 2%, 10%, 30%, 50%, 70%, and 90% of the peak flux. The Stokes I power values are expressed in units of kelvin (hereafter referred to as K).
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: (a) Gaussian fitting results with cuts along the major and minor axes for the central beam. Red plus signs and gray circles represent the nearest pixels to the straight lines passing through the major and minor axes, respectively. Contours (white solid lines) show intensity levels at 2%, 10%, 30%, 50%, 70%, and 90% of the peak flux. (b) Beam power data through a single antenna beam pattern. The cut along the major axis is represented by red plus signs with the corresponding Gaussian fit (red dashed line), while the minor axis cut is shown by gray circles with its Gaussian fit (gray solid line). The beam cuts are fairly symmetrical, consistent with the 2D symmetry of the central beam.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: Left: Fitted combined response of the 19 beams based on observation of J0854+2006 in Stokes I. The black solid lines are spaced 30° apart. Contours (black lines) depict intensities at levels of 1%, 2%, 5%, 10%, 30%, 50%, and 70% of the peak flux, respectively. The x- and y-axes represent the R.A. and decl. offsets relative to the center of beam M01 (see Table 2). Right: Simulated total intensity beam pattern of the 19 beams combined.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: (a) The log-normal combined with Gaussian fitting results with cuts along the major and minor axes for beam M08. The sidelobes are also well-fitted by a Gaussian distribution. Red plus signs and gray circles represent the nearest pixels to the straight lines passing through the major and minor axes, respectively. Contours (white solid lines) show intensity levels at 2%, 10%, 30%, 50%, 70%, and 90% of the peak flux. (b) Beam power data through a single antenna beam pattern. The cut along the major axis is represented by red plus signs. The red dashed line shows the fitting results including the log-normal fitting for the main lobe and the Gaussian fitting for the sidelobe. The cut along the minor axis is depicted by gray circles with its Gaussian fit (gray solid line). The vertical beam cut is fairly symmetrical and the horizontal cut is asymmetrical due to the sidelobe.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: Left: The telescope track during a raster scan along the decl. direction. Middle: The telescope track during a raster scan along the R.A. direction. Right: The overall telescope track during a raster scan. The x- and y-axes represent the R.A. and decl. offsets relative to the equatorial coordinates of J0854+2006 observed in 2021.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: Simulated Stokes I patterns of all 19 individual beams.
Paper: I-band Asymptotic Giant Branch Stars. I. Exploring a New Standard Candle for the Extragalactic Distance Scale 
Authors: Barry F. Madore, Wendy L. Freedman, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: The central region around the mode of the smoothed IAGB luminosity function for the LMC (rightmost panel: large, black dots, binned in 0.01 mag intervals) is well fit by the symmetric Gaussian shown in blue, having a dispersion of  ±0.20 mag around an apparent modal value of I = 14.16 mag. Given the sample size of 4204 IAGB stars (within 2σ of the mean), the error on the modal value is found to be  ±0.003 mag. The horizontal black line crossing the two panels, shows the mode of the IAGB. The horizontal yellow line below it marks the level of the TRGB for reference and comparison. One in ten stars are plotted in yellow so as to give a better sense of the density distribution along and across the RGB. All stars in the CMD redder than (V – I) = 2.5 mag are shown as red dots.
Paper: I-band Asymptotic Giant Branch Stars. I. Exploring a New Standard Candle for the Extragalactic Distance Scale 
Authors: Barry F. Madore, Wendy L. Freedman, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: I vs. (V – I) Color–magnitude diagram for the Large Magellanic Cloud. The newly identified AGB Plateau population of stars, discussed in this paper, is highlighted in black and yellow. Its flat luminosity function and unique color selection makes it an ideal candidate for being an extragalactic distance indicator.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Positional offsets in δ vary with color and magnitude at different decl. The top and bottom panels present the offsets as functions of color and magnitude, respectively. The triangles denote 3σ median positional discrepancies observed between the SDSS recorded galaxy positions and the established reference frame in different color/magnitude bins. The error bars are the corresponding standard deviation after 3σ clipping, reflecting the dispersion of the data points around the median. The curves are the best-fit polynomial. Blue and red represent the results before and after correction, respectively.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Left: CMD for Palomar 5, featuring all stars within the cluster radius of 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩14. The solid red curve delineates the theoretical isochrone, while the dashed red envelopes enclosing it symbolize a combined 1σ photometric uncertainty coupled with an intrinsic color error of 0.05 mag. To the right of the CMD, cyan circles accompanied by error bars illustrate the magnitude and color measurement uncertainties. The region enclosed by the dashed lines is used to select member stars. Middle: selected Gaia (black triangles) and non-Gaia (red triangles) member stars within the CMD. Right: proper-motion distribution of non-Gaia member stars. The median values for α* and δ are marked with solid red lines. The top and right panels present the distributions of ﹩{\mu }_{{\alpha }_{* }}﹩ and μδ, respectively.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Proper motions of quasars as functions of color (left panels) and magnitude (right panels). The top and bottom panels separately depict the α* and δ components. Each panel encompasses the full data set of 734,000 quasars. The red triangles with error bars represent the median and dispersion of each color or magnitude bin. The median and dispersion as a function of color and magnitude are also plotted in the middle and lower panels.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Corrected proper-motion distribution of distant halo stars, with solar motion effects accounted for correcting for the solar motion. The top and right panels present the histograms of ﹩{\mu }_{{\alpha }_{* }}﹩ and μδ, respectively. Red lines denote the median proper motion and corresponding standard deviations for α* and δ.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Left: histogram of galaxy numbers for all pixels. The dashed line shows the median value. Right: spatial distribution of galaxy numbers. The purple curve represents the Galactic plane.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Comparison of our proper motions with those from SDSS S82 for ﹩{\mu }_{{\alpha }_{* }}﹩ (left) and μδ (right). The red triangles with error bars represent the median and dispersion of each proper-motion bin. Red solid lines present the linear relationship of our and the S82 measurements, and the black dashed lines in the top and bottom panels mark y = x and y = 0, respectively.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Spatial distribution of the systematic (top panels) and random errors (bottom panels) with respect to galaxies. The left and right panels show the errors for α* and δ, respectively. The purple curves represent the Galactic plane.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Distribution of proper motions for quasars. The top and right panels present the histograms of ﹩{\mu }_{{\alpha }_{* }}﹩ and μδ, respectively. The red lines denote the median and standard deviation values for both the α* and δ components.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Spatial distribution of positional offsets (top panels) and offset errors (bottom panels). The left and right panels represent the distributions for α* and δ, respectively. The purple curves represent the Galactic plane.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Network structure of AE-Trans: input spectral data, pass through three convolutional layers (CNN encoder), and represent discriminative features with fewer channels. The output of the CNN encoder is decomposed into patches. These patches are reshaped into vectors and passed through a transformer encoder consisting of multi-head attention layers and MLP layers. Amplify and reshape the output of the transformer encoder to match the size of the abundance map, and use convolutional layers to reduce noise. Further use the softmax activation function to obtain the final abundance map. Finally, the decoder utilizes a single convolutional layer with weights as end data to reconstruct the represented hyperspectral image output.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Confusion matrix of AE-Trans test results on ACAD dataset: (a) unmixed endmember spectra, (b) the first row is the true abundance map and the second row is the display of unmixed abundance map.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Network structure of AAE-Net: the fusion of spectral data, differential extension data, and category information is input into an encoder consisting of three convolutional layers and three fully connected layers, and then input into a decoder composed of fully connected layers through a multi-head attention mechanism module. The category information is then fused and the albedo is output through the fully connected layers.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Comparison of the spectra of tested asteroids to the spectra of the simulated samples in their predicted classes.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Confusion matrix of AE-Trans test results on D. Korda et al.’s unmixed dataset (D. Korda et al. 2023b): (a) unmixed endmember spectra, (b) the first row is the true abundance map, and the second row displays the unmixed abundance map.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Comparison of the predicted albedo of asteroids with the albedo in the dataset. The blue dots represent the predicted albedo, and the red dots represent the dataset albedo.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Confusion matrix of ASC-Net test results on ASTD.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Confusion matrix of ASC-Net test results on VisNIR.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Spectral data of Eros (left) and Itokawa (right).
Paper: The Green Chile Project. I. A New Catalog of Low-redshift Extended Emission-line Nebulae
Authors: Audrey F. Dijeau, Moire K. M. Prescott, Kelly N. Sanderson
Figure caption: [O III]λ5007 luminosity vs. WISE 22 μm luminosity (νLν,W4 = ν F﹩{}_{\nu }4\pi {D}_{L}^{2}﹩, where DL is the luminosity distance). The dark purple circles are the Type 2 AGN from S. Yuan et al. (2016), presented for comparison. The blue stars are the GB sample (M. K. M. Prescott & K. N. Sanderson 2019). The pink triangles are the newly identified AGN-powered GCs with available [O III]λ5007 line measurements from SDSS/BOSS (A. S. Bolton et al. 2012).
Paper: The Green Chile Project. I. A New Catalog of Low-redshift Extended Emission-line Nebulae
Authors: Audrey F. Dijeau, Moire K. M. Prescott, Kelly N. Sanderson
Figure caption: Color–color plots showing simulated galaxies with SEDs defined as in the Bruzual–Charlot Atlas. Overlaid are the color selection criteria used in the original GB selection (M. Schirmer et al. 2013; black dashed lines). In the top panel, we also show our new color selection criteria.
Paper: The Green Chile Project. I. A New Catalog of Low-redshift Extended Emission-line Nebulae
Authors: Audrey F. Dijeau, Moire K. M. Prescott, Kelly N. Sanderson
Figure caption: Additional color–color plots of simulated galaxies with surrounding EELNs. Overlaid in the u − r vs. r − z plot (bottom panel) are the color cuts used in the original GB selection (M. Schirmer et al. 2013; black dashed lines).
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Integrated X-ray contours highlight the overall structure of the Stone MC. Top row: maximum X-ray brightness contour; bottom row: relative X-ray brightness contour (see Section 3.4 for more details). From left to right: branches and leaves of the H2CO (218.2 GHz) dendrogram colored by structure ID, CMZoom 1.3 mm continuum, X-ray 6.4 keV emission integrated from 2008–2017, Hi-GAL column density, and PPMAP column density.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Grouping structures with similar velocity ranges reveals an overall trend in the leaves seen in PPV space. Left panel: leaf indices 17, 18, 32, 33, 36, 37, 38, and 39. Middle panel: leaf indices 15, 19, 25, 26, 27, 30, 31, 34. Right panel: leaf indices 6, 10, 21, 24, and 28. Integrated X-ray contours are created based on the mean ﹩\overline{v}﹩ in Table 1 and shown as white contours in each panel (left: 2008, 2009, 2010; middle: 2011, 2013, 2015, 2016; right: 2017). Leaves 21 and 25 are not matched to any X-ray years, while leaves 10 and 24​​​​​ are not included in the analysis but are shown in case the reader is curious about their central velocities and projected positions.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Dendrogram leaves of the H2CO spectral line show good correspondence with X-ray contours. Structures colored from yellow to purple represent different structures that are correlated, while the structures in gray scale are unmatched with a particular feature in the X-ray. All dendrogram structures are seen in the H2CO spectral line within 30.2–73.8 km s−1. Contours A are drawn with thick lines, while Contours B are drawn with thin lines. For detailed information about the overlaid data sets and the velocity ranges for each dendrogram structure, see Table 1.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Line-of-sight coverage of existing Chandra observations at the projected distance of the Stone cloud, based on their starting date and duration. The parabolas follow Equation (1), assuming a 140 yr old event (as of 2008 January 1) with an infinitely short duration (top) and a 1 yr duration (bottom). The color indicates the observation year with the same color code as the X-ray contours, and existing observations not studied in this work are marked in gray. Finally, the shading gives an indication of the depth of the observations covering the plane.