adsabs/AstroCLIMB huggingface dataset:
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Temperature anisotropies in the E4 streamer belt solar wind. Panels (a) and (c) display the temperature anisotropy (T ⊥ p/T ∥p) signatures in the HPS solar wind, and panels (b) and (d) show the same parameters in the PCS solar wind. Panels (a) and (b) present the occurrence rates of temperature anisotropies in the HPS and PCS solar winds, respectively. Panels (c) and (d) exhibit the temperature anisotropy versus parallel plasma β (β ∥p) in the HPS and PCS solar winds, respectively. The different colored dashed lines are instabilities, as indicated by the legend, and the black line is the anticorrelation relationship. The red contours indicate 50% and 75% measurements.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Distributions of helium abundance (A He) vs. alpha–proton differential speed normalized by local Alfvén speed (ΔV  αp/V A) in the E4 streamer belt solar wind. Panels (a) and (b) present the helium characteristics in the HPS and PCS solar wind, respectively. The colors indicate the occurrence ratios. The red contours in both panels represent 50% and 75% of measurements.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Pressure variations in the E4 streamer belt solar wind. From top to bottom, the panels show the normalized e-PAD at energy of 346.5 eV, total pressure (P total) and expected total pressure (P expt), pressure components (P B, P e, and P p+a), normalized total pressure, and normalized pressure components. The three shaded regions and the blue dashed lines mark the high-β streamer belt solar wind and switchbacks, respectively, as in Figure 1.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Pressure variations in E4–E10. Panel (a) shows the distribution of normalized total pressure (P total Nor) vs. plasma β. Panel (b) shows the distribution of normalized thermal pressure (P  k  Nor) vs. normalized magnetic pressure (P  B  Nor). In both panels, the colors mean the occurrence ratios of the solar wind. The red and gold contours indicate the HPS and PCS solar winds, respectively. In panel (b), the cyan dashed line represents P B Nor + P k Nor = 45 nPa, and the black dashed line suggests P B Nor = P k Nor.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Radial evolution of the pressure components of all solar wind from E4 to E12 below 0.25 au. From top to bottom, rows (a)–(e) present the radial evolution of electron pressure P e, proton and alpha pressure P p+α , total kinetic pressure P k, magnetic pressure P B, and total pressure P total. In each row, the left panel shows the pressure component, with the color indicating the occurrence ratio of the data points. The black and blue lines represent the fitted results based on the mean and median values of the pressure component at each distance bin, respectively. The fitted evolution indices and correlated coefficients are presented accordingly. The middle and right panels show the fittings based on the four distance quantiles and four speed quantiles, respectively. In both panels, the red, blue, cyan, and brown lines indicate the fitting results according to the first (25%), second (50%), third (75%), and fourth (100%) quantiles, with the fitted evolution indices and correlated coefficients presented accordingly.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Overview of the high-β streamer belt solar wind from E5 to E10. In each figure, the panels from top to bottom show the normalized e-PAD at energy of 346.5 eV, plasma β, total and expected pressure, normalized total pressure, alpha-to-proton abundance ratio Na/Np, alpha–proton differential speed normalized by local Alfvén speed ΔVap/V A, and proton temperature anisotropy. The blue shaded regions mark the HPS solar wind, whereas the gray shaded regions mark the PCS solar wind.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Temperature anisotropy distributions of the PCS solar wind with different ΔV  αp/V A from E4 to E10. This figure has a similar format as the bottom panels of Figure 3.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Temperature anisotropies in the streamer belt solar wind from E4 to E10. This figure has the same format as Figure 3.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Distributions of parallel plasma β (β ∥p) vs. alpha–proton differential speed normalized by the local Alfvén speed (ΔV  αp/V A) in the E4 PCS solar wind. The colors indicate the occurrence ratios. The red contours represent 50% and 75% of measurements.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Distributions of helium abundance (A He) vs. alpha–proton differential speed normalized by local Alfvén speed (ΔV  αp/V A) in the streamer belt solar wind from E4 to E10. This figure has the same format as Figure 4.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Two-dimensional histograms depicting the spread of acceleration (left) and frequency (right) bin drift with peak power; color scale represents absolute count. Upper and lower red bars represent measured maximum and minimum values of the largest noise value in noise-only data samples.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Two-dimensional histograms depicting the spread of acceleration (left) and frequency (right) bin drift with peak power; color scale represents absolute count. Upper and lower red bars represent measured maximum and minimum values of the largest noise value in noise-only data samples. The arrays were searched for the peak in the opposite direction to Figure 10, leading to the skewing appearing on the other side of the acceleration axis. The extreme values cause the automatically generated bin edges to differ slightly to Figure 10.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Raw noise power histogram with ﹩{\chi }_{2}^{2}﹩ (=χ 2 with 2 d.o.f) comparison, linear scale (top). Raw noise power histogram with ﹩{\chi }_{2}^{2}﹩ comparison, log scale (middle). Percent difference between bfloat16 vs. single-precision bin count and double-precision vs. single-precision bin count (bottom). In all data series, N = 404,750,143 samples. Raw power (complex magnitude squared) is the internal measure of detection strength in AA (or PRESTO) before being converted to a significance level.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Graphs depicting the spread in peak power recreation between bfloat16 vs. single precision.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Graphs depicting acceleration (left) and frequency (right) bin drift between bfloat16 and single-precision results.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Fundamental peak acceleration (“z” bin) against bphase.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: GPU performance comparison with varying precision and input length (number of samples) in AstroAccelerate.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: The upper panel shows the distribution of ΔW2 (max−min) vs. the 6.7 GHz methanol maser variation index Var (Fmax/Fmin). The G24.33+0.14 is marked by the triangle, and the sources with large variations on both the 6.7 GHz methanol maser and W2 magnitude are marked by circles. The lower panel shows the distribution of the ΔW2 vs. the 6.7 GHz maser luminosity. The red and blue dots in both panels represent the secular and stochastic variables. The numbers in parentheses are the numbers of data points.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: W2 light curves of the episodic accretion candidates. Note that the red dashed line is the median W2 magnitude while the green dashed line denotes the criteria for both the burst and drop variables. The source ID, classification, and fitting results are given at the top of each panel.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: Comparisons of the cumulative distributions of the W1−W2 colors and W4 luminosities for different variable types. The luminosity is given in units of Jy pc2. The red, blue, and green solid curves represent the secular, stochastic, and nonvariable types, respectively.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: Comparisons of the cumulative distributions of the 6.7 GHz methanol maser luminosity (upper panel) and the variable index of the masers (lower panel) for secular, stochastic, and nonvariable classifications. The numbers in parentheses are the numbers of data points.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: Comparisons of the cumulative distributions of the different physical parameters between the two groups of secular variables classified according to the boundary limit of the periods. The red solid curve represents variables with periods of <3000 days, and the blue solid curve represents variables with periods of >3000 days.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: Comparisons of the cumulative distributions of the physical properties, dust temperature, bolometric luminosity, W1−W2 color, and W4 luminosity for different stochastic-type variables. The red, blue, and green solid curves represent the burst, drop, and irregular variables, respectively. The numbers in parentheses are the numbers of data points.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: The W2 light curves of the variables that can be matched to Olech et al. (2019, 2020, 2022). Note that the red dashed line is the median W2 magnitude while the green dashed line denotes the criteria for both the burst and drop variables. The source ID, classification, and fitting results are given at the top of each panel.
Paper: Sample and Statistical Analysis of the Near-Earth Object Wide-field Infrared Survey Explorer Variability of the 6.7 GHz Methanol Maser Sources
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, You-Xin Wang, Kai Yang, Dan Miao, Jiong-Heng Wu, Jun-Ting Liu, Yan-Kun Zhang
Figure caption: Cumulative distributions of the fractional amplitude and period for sin and sin+linear variables. The sin and sin+linear variables are represented by the red and blue solid curves, respectively.
Paper: The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: Quasar Properties from Data Releases 6 to 9
Authors: Jun-Jie Jin, Xue-Bing Wu, Yuming Fu, Su Yao, Yan-Li Ai, Xiao-Tong Feng, Zi-Qi He, Qin-Chun Ma, Yu-Xuan Pang, Rui Zhu, Yan-xia Zhang, Hai-long Yuan, Zhi-Ying Huo
Figure caption: The histograms of the monochromatic continuum luminosities (L 5100, L 1000, L 1300) and the estimated M BH (based on Hβ, Mg II, and C IV) for the LAMOST and S11 (R20) quasar sample. The mean value of each distribution is tabulated in the upper right corner.
Paper: The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: Quasar Properties from Data Releases 6 to 9
Authors: Jun-Jie Jin, Xue-Bing Wu, Yuming Fu, Su Yao, Yan-Li Ai, Xiao-Tong Feng, Zi-Qi He, Qin-Chun Ma, Yu-Xuan Pang, Rui Zhu, Yan-xia Zhang, Hai-long Yuan, Zhi-Ying Huo
Figure caption: Top panel: the distribution of the maximum magnitude difference based on SDSS and PS1 photometry ∣Δg∣ vs. time lag Δt. Bottom panel: the same distribution as in the top panel, but the observed-frame lag is switching to the rest-frame lag by dividing (1 + z).
Paper: The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: Quasar Properties from Data Releases 6 to 9
Authors: Jun-Jie Jin, Xue-Bing Wu, Yuming Fu, Su Yao, Yan-Li Ai, Xiao-Tong Feng, Zi-Qi He, Qin-Chun Ma, Yu-Xuan Pang, Rui Zhu, Yan-xia Zhang, Hai-long Yuan, Zhi-Ying Huo
Figure caption: An example for the LoBAL quasar. The top panel shows the whole spectrum, and the bottom panel is a zoom-in near the Mg II region. The blue line is the normal quasar template spectra at the same redshift. The Mg II absorption features are clear. There are no corrections for the redshift and Galactic extinction.
Paper: The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: Quasar Properties from Data Releases 6 to 9
Authors: Jun-Jie Jin, Xue-Bing Wu, Yuming Fu, Su Yao, Yan-Li Ai, Xiao-Tong Feng, Zi-Qi He, Qin-Chun Ma, Yu-Xuan Pang, Rui Zhu, Yan-xia Zhang, Hai-long Yuan, Zhi-Ying Huo
Figure caption: The redshift distributions of LAMOST (black) and SDSS (blue for S11, and red for R20) samples. The mean redshifts are tabulated in the upper right corner.
Paper: The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: Quasar Properties from Data Releases 6 to 9
Authors: Jun-Jie Jin, Xue-Bing Wu, Yuming Fu, Su Yao, Yan-Li Ai, Xiao-Tong Feng, Zi-Qi He, Qin-Chun Ma, Yu-Xuan Pang, Rui Zhu, Yan-xia Zhang, Hai-long Yuan, Zhi-Ying Huo
Figure caption: The HEALPix sky distributions of the quasars identified in LAMOST DR6−DR9 (panel (a)) and DR1−DR9 (panel (b)) are shown in equatorial coordinates with the parameters N side = 64 and area of 0.839 deg2 per pixel.
Paper: The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: Quasar Properties from Data Releases 6 to 9
Authors: Jun-Jie Jin, Xue-Bing Wu, Yuming Fu, Su Yao, Yan-Li Ai, Xiao-Tong Feng, Zi-Qi He, Qin-Chun Ma, Yu-Xuan Pang, Rui Zhu, Yan-xia Zhang, Hai-long Yuan, Zhi-Ying Huo
Figure caption: An example for the Lyα BAL quasar (black spectrum). The absorption features in the Lyα and C IV are obvious. The blue line is the BAL template spectra at the same redshift. There are no corrections for the redshift and Galactic extinction.
Paper: Image Super-resolution Methods for FY-3E X-EUVI 195 Å Solar Images
Authors: Qinglin Yang, Zhou Chen, Rongxin Tang, Xiaohua Deng, Jinsong Wang
Figure caption: We associate the reference image I  A  with the equivalent points of interest in I  B  and then transform I  B  to align the two images.
Paper: Image Super-resolution Methods for FY-3E X-EUVI 195 Å Solar Images
Authors: Qinglin Yang, Zhou Chen, Rongxin Tang, Xiaohua Deng, Jinsong Wang
Figure caption: We consider the same region as the X-EUVI 195 Å image, normalized using the extremum of a single sample on (a) and the common normalization on (b). Normalizing with extreme values preserves more image details.
Paper: Firefly: A Browser-based Interactive 3D Data Visualization Tool for Millions of Data Points
Authors: Alexander B. Gurvich, Aaron M. Geller
Figure caption: An illustration of the Firefly web application control flow at initialization. The steps outlined here are executed only once, in contrast to the components of the interactive render loop, which are repeated many times per second (illustrated in Figure C2). Major steps are in larger boxes and control flow proceeds from top to bottom. Substeps are in smaller boxes and proceed horizontally from left to right. Colors indicate which aspect of the application handles the step: viewer in black, UI in orange, and the optional octree build in purple (Appendix D). Major steps are executed sequentially, except for “generating the user interface” and “creating  three.js  particle mesh,” which occur in parallel.
Paper: Firefly: A Browser-based Interactive 3D Data Visualization Tool for Millions of Data Points
Authors: Alexander B. Gurvich, Aaron M. Geller
Figure caption: UI elements that affect the individual particle groups independently. The format of this figure is analogous to that of Figure A1.
Paper: Firefly: A Browser-based Interactive 3D Data Visualization Tool for Millions of Data Points
Authors: Alexander B. Gurvich, Aaron M. Geller
Figure caption: An illustration of the Firefly render loop control flow. The left shows a view of the overarching render loop flow while the right shows a zoomed-in view of the “update octree” step (described in Appendix D). Like Figure C1, major steps are in larger boxes, and substeps are in smaller boxes. Colors indicate which aspect of the application handles the step: viewer in black, UI in orange, and the optional octree steps in purple. Colored arrows indicate conditional branch outcomes where green indicates true, and red indicates false.
Paper: Firefly: A Browser-based Interactive 3D Data Visualization Tool for Millions of Data Points
Authors: Alexander B. Gurvich, Aaron M. Geller
Figure caption: UI elements that affect the application as a whole. Panes are organized hierarchically and are accessed by clicking labeled buttons (and the backwards arrow in the top left corner) to traverse the tree structure. Lime-green arrows connect buttons to the panes they open.
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Flowchart depicting the process of Fourier domain matched filtering using the overlap–save method on a GPU. Courtesy of Dimoudi et al. (2018).
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Relative difference between imaginary components of acceleration templates; color scale represents relative difference as in Equation (2).
Paper: Bits Missing: Finding Exotic Pulsars Using bfloat16 on NVIDIA GPUs
Authors: Jack White, Karel Adámek, Jayanta Roy, Sofia Dimoudi, Scott M. Ransom, Wesley Armour
Figure caption: Relative difference between real components of acceleration templates; color scale represents relative difference as in Equation (2).