Chin-Ping Hu (National Changhua University of Education/RIKEN); Teruaki Enoto (RIKEN); Toshio Terasawa (University of Tokyo/NAOJ); Shota Kisaka ( Hiroshima University); Sebastien Guillot (Institut de Recherche en Astrophysique); Natalia Lewandowska (Haverford College); Christian Malacaria (NASA); Paul S. Ray (U.S. Naval Research Laboratory); Wynn C.G. Ho (Haverford College); Alice K. Harding (NASA/GSFC); Takashi Okajima (NASA/GSFC); Zaven Arzoumanian (NASA/GSFC); Keith C. Gendreau (NASA/GSFC); ZorawarWadiasingh (NASA/GSFC); Craig B. Markwardt (NASA/GSFC); Yang Soong (NASA/GSFC); Steve Kenyon (NASA/GSFC); Slavko Bogdanov (Columbia University); Walid A. Majid (Caltech); Tolga Guver (Istanbul University); Gaurava K.Jaisawal (Technical University of Denmark); Rick Foster (MIT); Yasuhiro Murata (JAXA); Hiroshi Takeuchi (JAXA); Kazuhiro Takefuji (JAXA/NICT); Mamoru Sekido (NICT); Yoshinori Yonekura(Ibaraki University); HiroakiMisawa(Tohoku University); Fuminori Tsuchiya (Tohoku University); Takahiko Aoki (Yamaguchi University); Munetoshi Tokumaru (Nagoya University); Mareki Honma (NAOJ/University of Tokyo); Osamu Kameya (NAOJ); Tomoaki Oyama (NAOJ); KatsuakiAsano (University of Tokyo); Shinpei Shibata (Yamagata University); Shuta J. Tanaka (Aoyama Gakuin University)
Giant radio pulses (GRPs) are sporadic bursts emitted by some pulsars, lasting a few microseconds. GRPs are hundreds to thousands of times brighter than regular pulses from these sources. The only GRP-associated emission outside radio wavelengths is from the Crab Pulsar, where optical emission is enhanced by a few percent during GRPs. We observed the Crab Pulsar simultaneously at X-ray and radio wavelengths, finding enhancement of the X-ray emission by 3.8+/-0.7 % (a 5.4 sigma detection) coinciding with GRPs. This implies that the total emitted energy from GRPs is tens to hundreds of times higher than previously known. We discuss the implications for the pulsar emission mechanism and extragalactic fast radio bursts.