Aharonian Felix, Akamatsu Hiroki, Akimoto Fumie, Allen Steven W, Angelini Lorella, Audard Marc, Awaki Hisamitsu, Axelsson Magnus, Bamba Aya, Bautz Marshall W, Blandford Roger, Brenneman Laura W, Brown Gregory V, Bulbul Esra, Cackett Edward M, Chernyakova Maria, Chiao Meng P, Coppi Paolo S, Costantini Elisa, De Plaa Jelle, De Vries Cor P, Den Herder Jan-Willem, Done Chris, Dotani Tadayasu, Ebisawa Ken, Eckart Megan E, Enoto Teruaki, Ezoe Yuichiro, Fabian Andrew C, Ferrigno Carlo, Foster Adam R, Fujimoto Ryuichi, Fukazawa Yasushi, Furuzawa Akihiro, Galeazzi Massimiliano, Gallo Luigi C, Gandhi Poshak, Giustini Margherita, Goldwurm Andrea, Gu Liyi, Guainazzi Matteo, Haba Yoshito, Hagino Kouichi, Hamaguchi Kenji, Harrus Ilana M, Hatsukade Isamu, Hayashi Katsuhiro, Hayashi Takayuki, Hayashida Kiyoshi, Hiraga Junko S, Hornschemeier Ann, Hoshino Akio, Hughes John P, Ichinohe Yuto, Iizuka Ryo, Inoue Hajime, Inoue Yoshiyuki, Ishida Manabu, Ishikawa Kumi, Ishisaki Yoshitaka, Iwai Masachika, Kaastra Jelle, Kallman Tim, Kamae Tsuneyoshi, Kataoka Jun, Katsuda Satoru, Kawai Nobuyuki, Kelley Richard L, Kilbourne Caroline A, Kitaguchi Takao, Kitamoto Shunji, Kitayama Tetsu, Kohmura Takayoshi, Kokubun Motohide, Koyama Katsuji, Koyama Shu, Kretschmar Peter, Krimm Hans A, Kubota Aya, Kunieda Hideyo, Laurent Philippe, Lee Shiu-Hang, Leutenegger Maurice A, Limousin Olivier O, Loewenstein Michael, Long Knox S, Lumb David, Madejski Greg, Maeda Yoshitomo, Maier Daniel, Makishima Kazuo, Markevitch Maxim, Matsumoto Hironori, Matsushita Kyoko, Mccammon Dan, Mcnamara Brian R, Mehdipour Missagh, Miller Eric D, Miller Jon M, Mineshige Shin, Mitsuda Kazuhisa, Mitsuishi Ikuyuki, Miyazawa Takuya, Mizuno Tsunefumi, Mori Hideyuki, Mori Koji, Mukai Koji, Murakami Hiroshi, Mushotzky Richard F, Nakagawa Takao, Nakajima Hiroshi, Nakamori Takeshi, Nakashima Shinya, Nakazawa Kazuhiro, Nobukawa Kumiko K, Nobukawa Masayoshi, Noda Hirofumi, Odaka Hirokazu, Ohashi Takaya, Ohno Masanori, Okajima Takashi, Oshimizu Kenya, Ota Naomi, Ozaki Masanobu, Paerels Frits, Paltani Stéphane, Petre Robert, Pinto Ciro, Porter Frederick S, Pottschmidt Katja, Reynolds Christopher S, Safi-Harb Samar, Saito Shinya, Sakai Kazuhiro, Sasaki Toru, Sato Goro, Sato Kosuke, Sato Rie, Sawada Makoto, Schartel Norbert, Serlemtsos Peter J, Seta Hiromi, Shidatsu Megumi, Simionescu Aurora, Smith Randall K, Soong Yang, Stawarz Łukasz, Sugawara Yasuharu, Sugita Satoshi, Szymkowiak Andrew, Tajima Hiroyasu, Takahashi Hiromitsu, Takahashi Tadayuki, Takeda Shiníchiro, Takei Yoh, Tamagawa Toru, Tamura Takayuki, Tanaka Takaaki, Tanaka Yasuo, Tanaka Yasuyuki T, Tashiro Makoto S, Tawara Yuzuru, Terada Yukikatsu, Terashima Yuichi, Tombesi Francesco, Tomida Hiroshi, Tsuboi Yohko, Tsujimoto Masahiro, Tsunemi Hiroshi, Tsuru Takeshi Go, Uchida Hiroyuki, Uchiyama Hideki, Uchiyama Yasunobu, Ueda Shutaro, Ueda Yoshihiro, Uno Shiníchiro, Urry C Megan, Ursino Eugenio, Watanabe Shin, Werner Norbert, Wilkins Dan R, Williams Brian J, Yamada Shinya, Yamaguchi Hiroya, Yamaoka Kazutaka, Yamasaki Noriko Y, Yamauchi Makoto, Yamauchi Shigeo, Yaqoob Tahir, Yatsu Yoichi, Yonetoku Daisuke, Zhuravleva Irina, Zoghbi Abderahmen, Terasawa Toshio, Sekido Mamoru, Takefuji Kazuhiro, Kawai Eiji, Misawa Hiroaki, Tsuchiya Fuminori, Yamazaki Ryo, Kobayashi Eiji, Kisaka Shota, Aoki Takahiro
Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland.
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands.
Publ Astron Soc Jpn Nihon Tenmon Gakkai. 2018 Apr 11;70(2). doi: 10.1093/pasj/psx083.
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) ×10 erg cm, 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 > 0.02% brightening of the pulse-peak flux under such conditions.
为了寻找与蟹状脉冲星的巨型射电脉冲（GRPs）相关的巨型X射线脉冲，我们于2016年3月25日，在Hitomi任务失效之前，利用X射线卫星Hitomi在2 - 300 keV波段以及鹿岛宇宙通信观测所的射电天文台在1.4 - 1.7 GHz波段对蟹状脉冲星进行了同时观测，净曝光时间约为2千秒。Hitomi仪器的计时性能被证实满足计时要求，在主脉冲和间脉冲相位分别同时观测到约1000个和100个GRPs，并且我们发现在主脉冲或间脉冲相位中，巨型射电脉冲与X射线发射之间没有明显的相关性。所有变化都在脉冲峰值处X射线通量的2倍标准差波动范围内，在2 - 300 keV波段，主脉冲或间脉冲GRPs变化的3倍标准差上限分别为0.20相位宽度内峰值通量的22%或80%。当相位宽度限制在0.03相位时，主脉冲或间脉冲GRPs的值分别变为25%或110%。在Hitomi卫星的上限中，4.5 - 10 keV和70 - 300 keV波段的上限是首次获得，其他波段的上限与先前报告一致。在数值上，0.20相位宽度内主脉冲和间脉冲GRPs的上限分别约为(2.4和9.3)×10尔格·厘米。脉冲轮廓没有显著变化意味着GRPs起源于磁层内的局部位置，并且发射光子的粒子数量在时间上增加。然而，这些结果在统计上并不排除与GRPs相关的变化，因为在这种情况下，由于脉冲峰值通量亮度增加>0.02%，可能会出现X射线增强。
