Hitomi X-ray studies of Giant Radio Pulses from the Crab pulsar
Creators: name: Hitomi Collaboration
name: Aharonian, Felix
name: Akamatsu, Hiroki
name: Akimoto, Fumie
name: Allen, Steven W.
name: Angelini, Lorella
name: Audard, Marc
name: Awaki, Hisamitsu
name: Axelsson, Magnus
name: Bamba, Aya
name: Bautz, Marshall W.
name: Blandford, Roger
name: Brenneman, Laura W.
name: Brown, Gregory V.
name: Bulbul, Esra
name: Cackett, Edward M.
name: Chernyakova, Maria
name: Chiao, Meng P.
name: Coppi, Paolo S.
name: Costantini, Elisa
name: de Plaa, Jelle
name: de Vries, Cor P.
name: Herder, Jan-Willem den
name: Done, Chris
name: Dotani, Tadayasu
name: Ebisawa, Ken
name: Eckart, Megan E.
name: Enoto, Teruaki
name: Ezoe, Yuichiro
name: Fabian, Andrew C.
name: Ferrigno, Carlo
name: Foster, Adam R.
name: Fujimoto, Ryuichi
name: Fukazawa, Yasushi
name: Furuzawa, Akihiro
name: Galeazzi, Massimiliano
name: Gallo, Luigi C.
name: Gandhi, Poshak
name: Giustini, Margherita
name: Goldwurm, Andrea
name: Gu, Liyi
name: Guainazzi, Matteo
name: Haba, Yoshito
name: Hagino, Kouichi
name: Hamaguchi, Kenji
name: Harrus, Ilana M.
name: Hatsukade, Isamu
name: Hayashi, Katsuhiro
name: Hayashi, Takayuki
name: Hayashida, Kiyoshi
name: Hiraga, Junko S.
name: Hornschemeier, Ann
name: Hoshino, Akio
name: Hughes, John P.
name: Ichinohe, Yuto
name: Iizuka, Ryo
name: Inoue, Hajime
name: Inoue, Yoshiyuki
name: Ishida, Manabu
name: Ishikawa, Kumi
name: Ishisaki, Yoshitaka
name: Iwai, Masachika
name: Kaastra, Jelle
name: Kallman, Tim
name: Kamae, Tsuneyoshi
name: Kataoka, Jun
name: Katsuda, Satoru
name: Kawai, Nobuyuki
name: Kelley, Richard L.
name: Kilbourne, Caroline A.
name: Kitaguchi, Takao
name: Kitamoto, Shunji
name: Kitayama, Tetsu
name: Kohmura, Takayoshi
name: Kokubun, Motohide
name: Koyama, Katsuji
name: Koyama, Shu
name: Kretschmar, Peter
name: Krimm, Hans A.
name: Kubota, Aya
name: Kunieda, Hideyo
name: Laurent, Philippe
name: Lee, Shiu-Hang
name: Leutenegger, Maurice A.
name: Limousin, Olivier O.
name: Loewenstein, Michael
name: Long, Knox S.
name: Lumb, David
name: Madejski, Greg
name: Maeda, Yoshitomo
name: Maier, Daniel
name: Makishima, Kazuo
name: Markevitch, Maxim
name: Matsumoto, Hironori
name: Matsushita, Kyoko
name: McCammon, Dan
name: McNamara, Brian R.
name: Mehdipour, Missagh
name: Miller, Eric D.
name: Miller, Jon M.
name: Mineshige, Shin
name: Mitsuda, Kazuhisa
name: Mitsuishi, Ikuyuki
name: Miyazawa, Takuya
name: Mizuno, Tsunefumi
name: Mori, Hideyuki
name: Mori, Koji
name: Mukai, Koji
name: Murakami, Hiroshi
name: Mushotzky, Richard F.
name: Nakagawa, Takao
name: Nakajima, Hiroshi
name: Nakamori, Takeshi
name: Nakashima, Shinya
name: Nakazawa, Kazuhiro
name: Nobukawa, Kumiko K.
name: Nobukawa, Masayoshi
name: Noda, Hirofumi
name: Odaka, Hirokazu
name: Ohashi, Takaya
name: Ohno, Masanori
name: Okajima, Takashi
name: Oshimizu, Kenya
name: Ota, Naomi
name: Ozaki, Masanobu
name: Paerels, Frits
name: Paltani, Stéphane
name: Petre, Robert
name: Pinto, Ciro
name: Porter, Frederick S.
name: Pottschmidt, Katja
name: Reynolds, Christopher S.
name: Safi-Harb, Samar
name: Saito, Shinya
name: Sakai, Kazuhiro
name: Sasaki, Toru
name: Sato, Goro
name: Sato, Kosuke
name: Sato, Rie
name: Sawada, Makoto
name: Schartel, Norbert
name: Serlemtsos, Peter J.
name: Seta, Hiromi
name: Shidatsu, Megumi
name: Simionescu, Aurora
name: Smith, Randall K.
name: Soong, Yang
name: Stawarz, Ł ukasz
name: Sugawara, Yasuharu
name: Sugita, Satoshi
name: Szymkowiak, Andrew
name: Tajima, Hiroyasu
name: Takahashi, Hiromitsu
name: Takahashi, Tadayuki
name: Takeda, Shiníchiro
name: Takei, Yoh
name: Tamagawa, Toru
name: Tamura, Takayuki
name: Tanaka, Takaaki
name: Tanaka, Yasuo
name: Tanaka, Yasuyuki T.
name: Tashiro, Makoto S.
name: Tawara, Yuzuru
name: Terada, Yukikatsu
name: Terashima, Yuichi
name: Tombesi, Francesco
name: Tomida, Hiroshi
name: Tsuboi, Yohko
name: Tsujimoto, Masahiro
name: Tsunemi, Hiroshi
name: Tsuru, Takeshi Go
name: Uchida, Hiroyuki
name: Uchiyama, Hideki
name: Uchiyama, Yasunobu
name: Ueda, Shutaro
name: Ueda, Yoshihiro
name: Uno, Shiníchiro
name: Urry, C. Megan
name: Ursino, Eugenio
name: Watanabe, Shin
name: Werner, Norbert
name: Wilkins, Dan R.
name: Williams, Brian J.
name: Yamada, Shinya
name: Yamaguchi, Hiroya
name: Yamaoka, Kazutaka
name: Yamasaki, Noriko Y.
name: Yamauchi, Makoto
name: Yamauchi, Shigeo
name: Yaqoob, Tahir
name: Yatsu, Yoichi
name: Yonetoku, Daisuke
name: Zhuravleva, Irina
name: Zoghbi, Abderahmen
name: Terasawa, Toshio
name: Sekido, Mamoru
name: Takefuji, Kazuhiro
name: Kawai, Eiji
name: Misawa, Hiroaki
name: Tsuchiya, Fuminori
name: Yamazaki, Ryo
name: Kobayashi, Eiji
name: Kisaka, Shota
name: Aoki, Takahiro
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: To search for giant X-ray pulses correlated with the giant radio pulses (GRPs) from the Crab pulsar, we performed a simultaneous observation of the Crab pulsar with the X-ray satellite Hitomi in the 2 -- 300 keV band and the Kashima NICT radio observatory in the 1.4 -- 1.7 GHz band with a net exposure of about 2 ks on 25 March 2016, just before the loss of the Hitomi mission.The timing performance of the Hitomi instruments was confirmed to meet the timing requirement and about 1,000 and 100 GRPs were simultaneously observed at the main and inter-pulse phases, respectively, and we found no apparent correlation between the giant radio pulses and the X-ray emission in either the main or inter-pulse phases.All variations are within the 2 sigma fluctuations of the X-ray fluxes at the pulse peaks, and the 3 sigma upper limits of variations of main- or inter- pulse GRPs are 22\% or 80\% of the peak flux in a 0.20 phase width, respectively, in the 2 -- 300 keV band.The values become 25\% or 110\% for main or inter-pulse GRPs, respectively, when the phase width is restricted into the 0.03 phase.Among the upper limits from the Hitomi satellite, those in the 4.5-10 keV and the 70-300 keV are obtained for the first time, and those in other bands are consistent with previous reports.Numerically, the upper limits of main- and inter-pulse GRPs in the 0.20 phase width are about (2.4 and 9.3) $\times 10^{-11}$ erg cm$^{-2}$, respectively. No significant variability in pulse profiles implies that the GRPs originated from a local place within the magnetosphere and the number of photon-emitting particles temporally increases.However, the results do not statistically rule out variations correlated with the GRPs, because the possible X-ray enhancement may appear due to a $&gt;0.02$\% brightening of the pulse-peak flux under such conditions.
description: 18 pages, 7 figure, 6 tables, accepted for publication in PASJ