adsabs/AstroCLIMB huggingface dataset:
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: Schematic diagram of the Tlast determination method. Dwall and Eth represent the distance from the wall of the inner tank, and the energy threshold, respectively. A 20% random reduction is applied to simulate the expected signal loss due to spallation background rejection. The blue blocks indicate the flow of the Tlast determination method, while the green blocks represent the generated events.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: Background rate for the FV (orange), FV with spallation cut (violet), and outside FV (black) samples in SK. Background rates are generated according to M. Mori et al. (2022). In the present analysis, we use the background rate above 5 MeV following that study.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: An example scatter plot showing the visible energy of the observed events in SK as a function of time from the supernova explosion based on a single simulation. Signal events, represented by the orange points, and background events, represented by the gray points, are shown for the case with an energy threshold of 5 MeV. For signal events we use the Shen EOS with a 1.40M⊙ PNS mass. Panel (a) is assumed to be the full-volume observation, while panel (b) applies a spallation cut within the fiducial volume.
Paper: Lopsided and Bulging Distribution of Satellites around Paired Halos. II. 3D Analysis and Dependence on Projection and Selection Effects
Authors: Qinglin Ma, Cheng Li, Yanhan Guo
Figure caption: The same as the previous figure, but the panels from top to bottom are for halo pairs of different secondary-to-primary halo mass ratios, as indicated.
Paper: Lopsided and Bulging Distribution of Satellites around Paired Halos. II. 3D Analysis and Dependence on Projection and Selection Effects
Authors: Qinglin Ma, Cheng Li, Yanhan Guo
Figure caption: The same as the previous figure, but panels from top to bottom are for different secondary-to-primary halo mass ratios, as indicated.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: Backward-time analysis comparing different EOSs. The horizontal axis represents backward time, which sets the last observed event as the time origin, and the vertical axis represents the cumulative event number from that event. The black, red, blue, and green represent Shen EOS, LS220 EOS. Furusawa–Togashi EOS, and Togashi EOS, respectively. In both panels, the curves show the expected time evolution of the cumulative event number starting from Tlast. In panel (a), the timing uncertainties are evaluated with the time origin set at Tlast and are indicated by the error bars. In panel (b), the time origin is shifted to the 500th-to-last event (T500), and the error bars reflect the reduced timing uncertainties achieved by referencing this earlier event.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: Tlast distribution. The black, red, blue, and green lines represent Shen EOS, LS220 EOS. Furusawa–Togashi EOS, and Togashi EOS, respectively. The horizontal axis shows Tlast for each MC realization and the vertical axis shows the number of MC realizations in 1 s bins. The solid and grid lines in panel (b) mean a MZAMS = 15M⊙ and MZAMS = 40M⊙, respectively.