adsabs/AstroCLIMB huggingface dataset:
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Comparison of the percentages obtained in four different groups of the time intervals for (first column) long-duration radial IMF category, (second column) long-duration tangential IMF category, and (third column) long-duration normal IMF category, relative to the observation times of (top) 446 ICME events in 1995–2023 and (bottom) 865 SIR events in 1995–2016. (Group 1) The long-duration non-Parker spiral IMF events starting and ending within an ICME/an SIR interval. (Group 2) Those starting before an ICME/an SIR interval and ending within it. (Group 3) Those starting within an ICME/an SIR interval and ending after it. (Group 4) Those observed beyond any ICME/SIR intervals. The number of long-duration IMF events in each orientation type in 1995–2023 (N1995–2023) and in 1995–2016 (N1995–2016) are denoted in the corresponding panels.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Pitch angle distributions of the differential number flux (DNF) for ∼255 eV electrons for long-duration (duration ≥4 hr) events of (a) outward IMF, (b) inward IMF, (c) westward IMF, (d) eastward IMF, (e) northward IMF, and (f) southward IMF. The medians and upper/lower quartiles in eight local pitch angle bins (22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 wide) are plotted by circles and error bars, respectively. The number of data points available simultaneously in all pitch angle bins (nbin) is denoted in parentheses at the top of the panels. The values in the DNF are in units of 104/(cm2 s sr eV).
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: The percentages of the number of data points for radial, tangential, and normal IMF conditions (represented by the red, blue, and green bars, respectively) identified in the time intervals of (top) 446 ICME events in 1995–2023 and (bottom) 865 SIR events in 1995–2016. The total numbers of data points for non-Parker spiral IMF conditions in 1995–2023 (n1995–2023) and in 1995–2016 (n1995–2016) are denoted in the corresponding panels with different colors depending on the IMF orientation type.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: (a) The numbers of (1 hr resolution) Wind/MFI data available per year. (b) The numbers of Wind/MFI data available in two-dimensional bins of year and month. (c) The averages of the heliographic latitude (HLAT) of the Wind spacecraft in two-dimensional bins of year and month. All available Wind/MFI data are measured at PX-GSE ≥ +50 RE from 1995 to 2023, and the total number of them (n) is denoted in panel (a). In panels (a) and (b), the numbers of data points in 1995–2004 bins are not uniform and in general low relative to those in 2005–2023 bins, due mainly to the orbital characteristics of the spacecraft combined with the criteria for the spacecraft location applied to this study. In panel (c), we take the averages using only 1 hr resolution HLAT data at times the Wind/MFI data are available. Year–month bins for which the Wind/MFI data are not available are colored in cyan.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: The histograms of 1 hr difference (that is, ﹩\unicode{x02206}X\left(t\right){=}X\left(t\right){-}X(t{-}1\,{\mathrm{hr}})﹩) in (from left to right) bulk speed, number density, and temperature of the solar wind protons, alpha particle abundance, and IMF magnitude for (first–third rows) long-duration (duration ≥ 4 hr) radial, tangential, and normal IMF events. The total numbers of time-differenced data for Wind/SWE with protons (nSWE,p), Wind/SWE with both protons and alpha particles (nSWE,p&α), and Wind/MFI (nMFI) used in each of unsigned IMF categories are denoted in the first, fourth, and fifth column panels, respectively. In each panel, the median and upper/lower quartiles are plotted by the vertical black solid line and two vertical black dashed lines, respectively, and the corresponding values are also provided in the panel. The thick vertical gray solid line indicates zero value in the corresponding units. The bars on both edges of each histogram shows the percentages containing the numbers of data points with values beyond the range of the domain.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Occurrence rates of (a) outward IMF, (b) inward IMF, (c) westward IMF, (d) eastward IMF, (e) northward IMF, and (f) southward IMF, in two-dimensional bins of year and month. The values are displayed in percentages. In each panel, the total number of data points used in the corresponding IMF configuration type is denoted by n in parentheses. The year–month bins for which the Wind/MFI data are not available are colored in cyan (also see Figure 1(b)). The solar maximum phases (in 2000–2002 and 2013–2015) and solar minimum phases (in 1995–1997, 2007–2009, and 2018–2020) are denoted as the red and blue horizontal bars, respectively, on the top of each panel.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Histograms of (from left to right) bulk speed, number density, and temperature of the solar wind protons, alpha particle abundance, and the IMF magnitude measured at PX-GSE ≥ +50 RE by the Wind spacecraft for various time intervals. (First row) The whole period of interest (1995–2023). (Second–fourth rows) The intervals of long-duration (duration ≥ 4 hr) radial, tangential, and normal IMF events. For each of the various time intervals, the total number of Wind/SWE data points available for protons is denoted by nSWE,p in the first column panels, and that for both protons and alpha particles is denoted by nSWE,p&α in the fourth column panels. The total number of Wind/MFI data points available is denoted by nMFI in the fifth column panels. The median and upper/lower quartiles of each data set are overplotted in the histogram by the vertical black solid line and two vertical black dashed lines, respectively. These values are also denoted in each panel. A rightmost bar in each histogram shows the percentage containing the number of data points with values beyond the range of the domain.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Yearly variations of the occurrence rate (plotted as bars in percentages) for (a) unsigned radial IMF, (b) unsigned tangential IMF, and (c) unsigned normal IMF, observed by the Wind spacecraft in 1995–2023. In each panel, the total number of data points (n) used in the corresponding IMF configuration type is given in parentheses. The yearly averages of the adjusted F10.7 index are overplotted as the open circles. The red and blue horizontal bars on the top indicate solar maximum phases (in 2000–2002 and 2013–2015) and minimum phases (in 1995–1997, 2007–2009, and 2018–2020), respectively, defined as 3 yr centered at the local maxima and local minima of the adjusted F10.7 index. The linear Pearson correlation coefficient between the occurrence rate of the corresponding IMF configurations and the adjusted F10.7 index is denoted by CC.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: (a)–(c) Distributions of duration (plotted as bars) for the events of unsigned radial IMF, unsigned tangential IMF, and unsigned normal IMF. (d)–(i) Distributions of duration for the events of signed radial (outward/inward) IMF, signed tangential (westward/eastward) IMF, and signed normal (northward/southward) IMF. The cumulative rates of the number of events with durations are plotted in percentages by open circles. The events with durations of no less than 4 hr (vertical dashed lines) are selected as long-duration (duration ≥ 4 hr) non-Parker spiral IMF events. The total number of events (NTotal) and the number of long-duration events (Nt ≥ 4 hr) for individual IMF configuration categories are denoted in each panel. The numbers of data points (n) for all events and long-duration events are denoted in parentheses below NTotal and Nt ≥ 4 hr, respectively.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: The network architecture of GC-SWGAN. The symbol z represents the input random noise vector used by the generator to produce synthetic images. Xunlabeled denotes the input unlabeled real images, Xlabeled indicates the input labeled real images, and Xfake represents the synthetic images generated by the generator G. The generator G employs a multilayer convolutional network structure, responsible for generating synthetic images that resemble real images. The task of the discriminator D is to distinguish between real and fake images, differentiating real images from those generated by the generator. The classifier C aims to learn how to assign correct class labels to real samples. In this study, the classifier C focuses on differentiating real samples as ringed galaxies and nonringed galaxies.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Classification performance of the model for ringed galaxies. Left panel: the ROC of the model on the training data and test data. The embedded subplot shows the x-axis on a logarithmic scale. The black dashed line represents the ROC curve for the training set, while the orange solid line indicates the ROC curve for the test set. The dotted navy line represents the performance benchmark of a random classifier (AU-ROC = 0.5). Right panel: the PRC of the model’s classifier. The meaning of the lines is consistent with that of the left panel. The values on the curve represent different classification thresholds for ringed galaxies.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Frequency histograms of three samples (input total galaxies, ring galaxies identified by the model, and ring galaxies used for training) for galaxy redshift z (left panel) and DESI r-band apparent magnitude mr (right panel). The solid red line represents model-predicted ring galaxies, the dashed blue line represents all input galaxies, and the dotted black line represents ringed galaxies used in model training.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Relationship between the probability of the model classifying a galaxy as a ringed galaxy and the apparent magnitude mr (left panel) and redshift (right panel). Each point represents the median probability within the corresponding magnitude interval (left panel) or redshift interval (right panel), with error bars indicating the range from the 25th to the 75th percentile.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Images of 30 random galaxies from the catalog of 62,962 ringed galaxies detected by the model. The red numbers in each panel indicate the probability of being predicted as a ringed galaxy.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Random samples of galaxies without rings from our training set.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Random samples of galaxies with rings from our training set.
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Distributions of redshift, Mr, Mg − Mr, and ﹩{\rm{Log}}({\rm{SSFR}})﹩ for ringed galaxies (solid red lines) and for the control samples (nonringed galaxies; dashed black lines). Panels (a) and (b) demonstrate that the control galaxy sample exhibits high similarity to the ringed galaxy sample in terms of redshift distribution and r-band absolute magnitude (Mr). In contrast, panels (c) and (d) reveal significant differences between the control samples and ringed galaxies in the distributions of g − r color and specific star formation rate (SSFR).
Paper: Detecting Galactic Rings in the DESI Legacy Imaging Surveys with Semisupervised Deep Learning
Authors: Jianzhen Chen, Zhijian Luo, Cheng Cheng, Jun Hou, Shaohua Zhang, Chenggang Shu
Figure caption: Images of 10 random galaxies predicted by the model to have ring structures. All these galaxies have 0.20 < z < 0.25 and 16.5 < mr < 17. The red numbers in each panel indicate the probability of being predicted as a ringed galaxy.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: Transmittance of the CIBER-2 filters. The solid lines represent the transmittance of the window pane filters, while the dashed lines show the transmittance of the LVFs, multiplied by the transmittance of the beam splitters and order sort filters, which determine the bandpass wavelengths. The LVF transmittance shown corresponds to the wavelength of peak transmittance of each detector column. The transmittance values presented are at room temperature.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: Design of the end-to-end optical chain consisting of the telescope and the relay lens optics with the light beams (blue, green, and red lines). Each lens optics for the three photometric bands, arm S, arm M, and arm L, is shown separately. The G1 lens is common to all photometric bands. The light from G1 is split into two beams for arm S/arm M and arm L by a dichroic beam splitter BS1. The shorter wavelength light is collimated by the lens unit consisting of G2, G3, and G4 and split into two beams for the arm S and arm M focusing by another dichroic beam splitter BS2. The final lens system for each wavelength band focuses the beam onto the detector. The order-sorting filter to block out-of-band light is placed in front of the focusing optics for each band. The window pane filter and the linear-variable filter are placed close to the detector surface.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: (Left) Positions of science fields projected on the ecliptic sphere. Target fields optimized for assessing foregrounds (blue points) and those optimized for intensity mapping (orange points) are visible from WSMR between November and July of each year (white area). The extragalactic fields we consider (ELAIS-N1; north ecliptic pole, NEP; Bootes; Lockman; and COSMOS) have been surveyed extensively in the near-IR and have ample ancillary data for masking and cross correlation. (Right) A typical flight plan for CIBER-2 modeled on flight 36.281. The dashed green curve shows the payload’s altitude versus time. Calibration lamp data is taken during ascent (orange zone), and optically dark data is taken during descent (gray zone).
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: Typical CIBER-2 thermal cycle showing four of two dozen thermometers that are monitored by ground equipment during laboratory testing. The cooling cycle is computer controlled so that dT/dt < 1 K minute−1 to account for the differential thermal contraction of the metal and glass optical assembly. After 24 hr, the nitrogen tank can be filled, and it must be refilled every 6 hr as the optical assembly cools. The optics reach a steady-state temperature, and the instrument can be tested 54 hr after the first fill. Finally, the warming cycle takes about 48 hr from fully cold to ambient temperature. In this thermal cycle, a small amount of nitrogen gas was injected into the vacuum section to improve conduction to room temperature at 120 hr.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: The overall structure of the CIBER-2 payload. The upper panel shows a partial section of the instrument section in observing configuration with the door open and pop-up baffle deployed. The rocket skin sections forward of the experiment have been suppressed. The lower panel shows the cryogenic insert in partial section, highlighting the telescope and imaging optics described in Section 3.1. The optics couple to three focal plane assemblies (Section 3.4), one of which is shown separated from the optics for clarity.