Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer
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AHARONIAN, F.; H. AKAMATSU; F. AKIMOTO; S.W. ALLEN; L. ANGELINI; M. AUDARD; H. AWAKI; M. AXELSSON; A. BAMBA; M.W. BAUTZ; R. BLANDFORD; L.W. BRENNEMAN; GV. BROWN; E. BULBUL; EM. CACKETT; M. CHERNYAKOVA; MP CHIAO; P.S. COPPI; E. COSTANTINI; J. DE PLAA; C.P. DE VRIES; J.W. DEN HERDER; C. DONE; T. DOTANI; K. EBISAWA; ME. ECKART; T. ENOTO; Y. EZOE; A.C. FABIAN; C. FERRIGNO; A.R. FOSTER; R. FUJIMOTO; Y. FUKAZAWA; A. FURUZAWA; M. GALEAZZI; L.C. GALLO; P. GANDHI; M. GIUSTINI; A. GOLDWURM; Gu LY; M. GUAINAZZI; Y. HABA; K. HAGINO; K. HAMAGUCH; IM. HARRUS; I. HATSUKADE; K. HAYASHI; T. HAYASHI; K. HAYASHIDA; JS HIRAGA; A. HORNSCHEMEIER; A. HOSHINO; J.P. HUGHES; Y. ICHINOHE; R. IIZUKA; H. INOUE; Y. INOUE; M. ISHIDA; K. ISHIKAWA; Y. ISHISAKI; J. KAASTRA; T. KALLMAN; T. KAMAE; J. KATAOKA; S. KATSUDA; N. KAWAI; R.L. KELLEY; C.A. KILBOURNE; T. KITAGUCHI; S. KITAMOTO; T. KITAYAMA; T. KOHMURA; M. KOKUBUN; K. KOYAMA; S. KOYAMA; P. KRETSCHMAR; HA KRIMM; A. KUBOTA; H. KUNIEDA; P. LAURENT; SH. LEE; M.A. LEUTENEGGER; O. LIMOUSIN; M. LOEWENSTEIN; K.S. LONG; D. LUMB; G. MADEJSKI; Y. MAEDA; D. MAIER; K. MAKISHIMA; M. MARKEVITCH; H. MATSUMOTO; K. MATSUSHITA; D. MCCAMMON; B.R. MCNAMARA; M. MEHDIPOUR; E.D. MILLER; J.M. MILLER; S. MINESHIGE; K. MITSUDA; I. MITSUISHI; T. MIYAZAWA; T. MIZUNO; H. MORI; K. MORI; K. MUKAI; H. MURAKAMI; R.F. MUSHOTZKY; T. NAKAGAWA; H. NAKAJIMA; T. NAKAMORI; S. NAKASHIMA; K. NAKAZAWA; KK NOBUKAWA; M. NOBUKAWA; H. NODA; H. ODAKA; T. OHASHI; M. OHNO; T. OKAJIMA; N. OTA; M. OZAKI; F. PAERELS; S. PALTANI; R. PETRE; C. PINTO; F.S. PORTER; K. POTTSCHMIDT; C.S. REYNOLDS; S. SAFI-HARB; S. SAITO; K. SAKAI; T. SASAKI; G. SATO; K. SATO; R. SATO; T. SATO; M. SAWADA; N. SCHARTEL; P.J. SERLEMTSOS; H. SETA; M. SHIDATSU; A. SIMIONESCU; R.K. SMITH; Y. SOONG; L. STAWARZ; Y. SUGAWARA; S. SUGITA; A. SZYMKOWIAK; H. TAJIMA; H. TAKAHASHI; T. TAKAHASHI; S. TAKEDA; Y. TAKEI; T. TAMAGAWA; T. TAMURA; T. TANAKA; Y. TANAKA; YT TANAKA; MS TASHIRO; Y. TAWARA; Y. TERADA; Y. TERASHIMA; F. TOMBESI; H. TOMIDA; Y. TSUBOI; M. TSUJIMOTO; H. TSUNEMI; TG TSURU; H. UCHIDA; H. UCHIYAMA; Y. UCHIYAMA; S. UEDA; Y. UEDA; S. UNO; CM URRY; E. URSINO; S. WATANABE; Norbert WERNER; D.R. WILKINS; B.J. WILLIAMS; S. YAMADA; H. YAMAGUCHI; K. YAMAOKA; N.Y. YAMASAKI; M. YAMAUCHI; S. YAMAUCHI; T. YAQOOB; Y. YATSU; D. YONETOKU; I. ZHURAVLEVA; A. ZOGHBI; N. TOMINAGA a TJ MORIYA
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, OXFORD, OXFORD UNIV PRESS, 2018, 0004-6264
The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054 AD. When viewed as a supernova remnant (SNR), it has an anomalously low observed ejecta mass and kinetic energy for an Fe-core-collapse SN. Intensive searches have been made for a massive shell that solves this discrepancy, but none has been detected. An alternative idea is that SN 1054 is an electron-capture (EC) explosion with a lower explosion energy by an order of magnitude than Fe-core-collapse SNe. X-ray imaging searches were performed for the plasma emission from the shell in the Crab outskirts to set a stringent upper limit on the X-ray emitting mass. However, the extreme brightness of the source hampers access to its vicinity. We thus employed spectroscopic technique using the X-ray micro-calorimeter on board the Hitomi satellite. By exploiting its superb energy resolution, we set an upper limit for emission or absorption features from as yet undetected thermal plasma in the 2-12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data. By assembling these results, a new upper limit was obtained for the X-ray plasma mass of less than or similar to 1 M-circle dot for a wide range of assumed shell radius, size, and plasma temperature values both in and out of collisional equilibrium. To compare with the observation, we further performed hydrodynamic simulations of the Crab SNR for two SN models (Fe-core versus EC) under two SN environments (uniform interstellar medium versus progenitor wind). We found that the observed mass limit can be compatible with both SN models if the SN environment has a low density of less than or similar to 0.03 cm(-3) (Fe core) or less than or similar to 0.1 cm(-3) (EC) for the uniform density, or a progenitor wind density somewhat less than that provided by amass loss rate of 10(-5) M-circle dot yr(-1) at 20 km s(-1) for the wind environment.
AHARONIAN, F.; H. AKAMATSU; F. AKIMOTO; S.W. ALLEN; L. ANGELINI; M. AUDARD; H. AWAKI; M. AXELSSON; A. BAMBA; M.W. BAUTZ; R. BLANDFORD; L.W. BRENNEMAN; GV. BROWN; E. BULBUL; EM. CACKETT; M. CHERNYAKOVA; MP CHIAO; P.S. COPPI; E. COSTANTINI; J. DE PLAA; C.P. DE VRIES; J.W. DEN HERDER; C. DONE; T. DOTANI; K. EBISAWA; ME. ECKART; T. ENOTO; Y. EZOE; A.C. FABIAN; C. FERRIGNO; A.R. FOSTER; R. FUJIMOTO; Y. FUKAZAWA; A. FURUZAWA; M. GALEAZZI; L.C. GALLO; P. GANDHI; M. GIUSTINI; A. GOLDWURM; Gu LY; M. GUAINAZZI; Y. HABA; K. HAGINO; K. HAMAGUCH; IM. HARRUS; I. HATSUKADE; K. HAYASHI; T. HAYASHI; K. HAYASHIDA; JS HIRAGA; A. HORNSCHEMEIER; A. HOSHINO; J.P. HUGHES; Y. ICHINOHE; R. IIZUKA; H. INOUE; Y. INOUE; M. ISHIDA; K. ISHIKAWA; Y. ISHISAKI; J. KAASTRA; T. KALLMAN; T. KAMAE; J. KATAOKA; S. KATSUDA; N. KAWAI; R.L. KELLEY; C.A. KILBOURNE; T. KITAGUCHI; S. KITAMOTO; T. KITAYAMA; T. KOHMURA; M. KOKUBUN; K. KOYAMA; S. KOYAMA; P. KRETSCHMAR; HA KRIMM; A. KUBOTA; H. KUNIEDA; P. LAURENT; SH. LEE; M.A. LEUTENEGGER; O. LIMOUSIN; M. LOEWENSTEIN; K.S. LONG; D. LUMB; G. MADEJSKI; Y. MAEDA; D. MAIER; K. MAKISHIMA; M. MARKEVITCH; H. MATSUMOTO; K. MATSUSHITA; D. MCCAMMON; B.R. MCNAMARA; M. MEHDIPOUR; E.D. MILLER; J.M. MILLER; S. MINESHIGE; K. MITSUDA; I. MITSUISHI; T. MIYAZAWA; T. MIZUNO; H. MORI; K. MORI; K. MUKAI; H. MURAKAMI; R.F. MUSHOTZKY; T. NAKAGAWA; H. NAKAJIMA; T. NAKAMORI; S. NAKASHIMA; K. NAKAZAWA; KK NOBUKAWA; M. NOBUKAWA; H. NODA; H. ODAKA; T. OHASHI; M. OHNO; T. OKAJIMA; N. OTA; M. OZAKI; F. PAERELS; S. PALTANI; R. PETRE; C. PINTO; F.S. PORTER; K. POTTSCHMIDT; C.S. REYNOLDS; S. SAFI-HARB; S. SAITO; K. SAKAI; T. SASAKI; G. SATO; K. SATO; R. SATO; T. SATO; M. SAWADA; N. SCHARTEL; P.J. SERLEMTSOS; H. SETA; M. SHIDATSU; A. SIMIONESCU; R.K. SMITH; Y. SOONG; L. STAWARZ; Y. SUGAWARA; S. SUGITA; A. SZYMKOWIAK; H. TAJIMA; H. TAKAHASHI; T. TAKAHASHI; S. TAKEDA; Y. TAKEI; T. TAMAGAWA; T. TAMURA; T. TANAKA; Y. TANAKA; YT TANAKA; MS TASHIRO; Y. TAWARA; Y. TERADA; Y. TERASHIMA; F. TOMBESI; H. TOMIDA; Y. TSUBOI; M. TSUJIMOTO; H. TSUNEMI; TG TSURU; H. UCHIDA; H. UCHIYAMA; Y. UCHIYAMA; S. UEDA; Y. UEDA; S. UNO; CM URRY; E. URSINO; S. WATANABE; Norbert WERNER; D.R. WILKINS; B.J. WILLIAMS; S. YAMADA; H. YAMAGUCHI; K. YAMAOKA; N.Y. YAMASAKI; M. YAMAUCHI; S. YAMAUCHI; T. YAQOOB; Y. YATSU; D. YONETOKU; I. ZHURAVLEVA; A. ZOGHBI; N. TOMINAGA a TJ MORIYA. Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN. OXFORD: OXFORD UNIV PRESS, 2018, roč. 70, č. 2, s. "14-1"-"14-17", 17 s. ISSN 0004-6264. Dostupné z: https://doi.org/10.1093/pasj/psx072.
@article{1444338, author = {Aharonian, F. and Akamatsu, H. and Akimoto, F. and Allen, S.W. and Angelini, L. and Audard, M. and Awaki, H. and Axelsson, M. and Bamba, A. and Bautz, M.W. and Blandford, R. and Brenneman, L.W. and Brown, GV. and Bulbul, E. and Cackett, EM. and Chernyakova, M. and Chiao, MP and Coppi, P.S. and Costantini, E. and de Plaa, J. and de Vries, C.P. and den Herder, J.W. and Done, C. and Dotani, T. and Ebisawa, K. and Eckart, ME. and Enoto, T. and Ezoe, Y. and Fabian, A.C. and Ferrigno, C. and Foster, A.R. and Fujimoto, R. and Fukazawa, Y. and Furuzawa, A. and Galeazzi, M. and Gallo, L.C. and Gandhi, P. and Giustini, M. and Goldwurm, A. and LY, Gu and Guainazzi, M. and Haba, Y. and Hagino, K. and Hamaguch, K. and Harrus, IM. and Hatsukade, I. and Hayashi, K. and Hayashi, T. and Hayashida, K. and Hiraga, JS and Hornschemeier, A. and Hoshino, A. and Hughes, J.P. and Ichinohe, Y. and Iizuka, R. and Inoue, H. and Inoue, Y. and Ishida, M. and Ishikawa, K. and Ishisaki, Y. and Kaastra, J. and Kallman, T. and Kamae, T. and Kataoka, J. and Katsuda, S. and Kawai, N. and Kelley, R.L. and Kilbourne, C.A. and Kitaguchi, T. and Kitamoto, S. and Kitayama, T. and Kohmura, T. and Kokubun, M. and Koyama, K. and Koyama, S. and Kretschmar, P. and Krimm, HA and Kubota, A. and Kunieda, H. and Laurent, P. and Lee, SH. and Leutenegger, M.A. and Limousin, O. and Loewenstein, M. and Long, K.S. and Lumb, D. and Madejski, G. and Maeda, Y. and Maier, D. and Makishima, K. and Markevitch, M. and Matsumoto, H. and Matsushita, K. and McCammon, D. and McNamara, B.R. and Mehdipour, M. and Miller, E.D. and Miller, J.M. and Mineshige, S. and Mitsuda, K. and Mitsuishi, I. and Miyazawa, T. and Mizuno, T. and Mori, H. and Mori, K. and Mukai, K. and Murakami, H. and Mushotzky, R.F. and Nakagawa, T. and Nakajima, H. and Nakamori, T. and Nakashima, S. and Nakazawa, K. and Nobukawa, KK and Nobukawa, M. and Noda, H. and Odaka, H. and Ohashi, T. and Ohno, M. and Okajima, T. and Ota, N. and Ozaki, M. and Paerels, F. and Paltani, S. and Petre, R. and Pinto, C. and Porter, F.S. and Pottschmidt, K. and Reynolds, C.S. and SafiandHarb, S. and Saito, S. and Sakai, K. and Sasaki, T. and Sato, G. and Sato, K. and Sato, R. and Sato, T. and Sawada, M. and Schartel, N. and Serlemtsos, P.J. and Seta, H. and Shidatsu, M. and Simionescu, A. and Smith, R.K. and Soong, Y. and Stawarz, L. and Sugawara, Y. and Sugita, S. and Szymkowiak, A. and Tajima, H. and Takahashi, H. and Takahashi, T. and Takeda, S. and Takei, Y. and Tamagawa, T. and Tamura, T. and Tanaka, T. and Tanaka, Y. and Tanaka, YT and Tashiro, MS and Tawara, Y. and Terada, Y. and Terashima, Y. and Tombesi, F. and Tomida, H. and Tsuboi, Y. and Tsujimoto, M. and Tsunemi, H. and Tsuru, TG and Uchida, H. and Uchiyama, H. and Uchiyama, Y. and Ueda, S. and Ueda, Y. and Uno, S. and Urry, CM and Ursino, E. and Watanabe, S. and Werner, Norbert and Wilkins, D.R. and Williams, B.J. and Yamada, S. and Yamaguchi, H. and Yamaoka, K. and Yamasaki, N.Y. and Yamauchi, M. and Yamauchi, S. and Yaqoob, T. and Yatsu, Y. and Yonetoku, D. and Zhuravleva, I. and Zoghbi, A. and Tominaga, N. and Moriya, TJ}, article_location = {OXFORD}, article_number = {2}, doi = {https://doi.org/10.1093/pasj/psx072}, keywords = {instrumentation: spectrographs; ISM: individual (Crab nebula); ISM: supernova remnants; methods: observational}, language = {eng}, issn = {0004-6264}, journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN}, title = {Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer}, url = {https://arxiv.org/pdf/1707.00054.pdf}, volume = {70}, year = {2018} }
TY - JOUR ID - 1444338 AU - Aharonian, F. - Akamatsu, H. - Akimoto, F. - Allen, S.W. - Angelini, L. - Audard, M. - Awaki, H. - Axelsson, M. - Bamba, A. - Bautz, M.W. - Blandford, R. - Brenneman, L.W. - Brown, GV. - Bulbul, E. - Cackett, EM. - Chernyakova, M. - Chiao, MP - Coppi, P.S. - Costantini, E. - de Plaa, J. - de Vries, C.P. - den Herder, J.W. - Done, C. - Dotani, T. - Ebisawa, K. - Eckart, ME. - Enoto, T. - Ezoe, Y. - Fabian, A.C. - Ferrigno, C. - Foster, A.R. - Fujimoto, R. - Fukazawa, Y. - Furuzawa, A. - Galeazzi, M. - Gallo, L.C. - Gandhi, P. - Giustini, M. - Goldwurm, A. - LY, Gu - Guainazzi, M. - Haba, Y. - Hagino, K. - Hamaguch, K. - Harrus, IM. - Hatsukade, I. - Hayashi, K. - Hayashi, T. - Hayashida, K. - Hiraga, JS - Hornschemeier, A. - Hoshino, A. - Hughes, J.P. - Ichinohe, Y. - Iizuka, R. - Inoue, H. - Inoue, Y. - Ishida, M. - Ishikawa, K. - Ishisaki, Y. - Kaastra, J. - Kallman, T. - Kamae, T. - Kataoka, J. - Katsuda, S. - Kawai, N. - Kelley, R.L. - Kilbourne, C.A. - Kitaguchi, T. - Kitamoto, S. - Kitayama, T. - Kohmura, T. - Kokubun, M. - Koyama, K. - Koyama, S. - Kretschmar, P. - Krimm, HA - Kubota, A. - Kunieda, H. - Laurent, P. - Lee, SH. - Leutenegger, M.A. - Limousin, O. - Loewenstein, M. - Long, K.S. - Lumb, D. - Madejski, G. - Maeda, Y. - Maier, D. - Makishima, K. - Markevitch, M. - Matsumoto, H. - Matsushita, K. - McCammon, D. - McNamara, B.R. - Mehdipour, M. - Miller, E.D. - Miller, J.M. - Mineshige, S. - Mitsuda, K. - Mitsuishi, I. - Miyazawa, T. - Mizuno, T. - Mori, H. - Mori, K. - Mukai, K. - Murakami, H. - Mushotzky, R.F. - Nakagawa, T. - Nakajima, H. - Nakamori, T. - Nakashima, S. - Nakazawa, K. - Nobukawa, KK - Nobukawa, M. - Noda, H. - Odaka, H. - Ohashi, T. - Ohno, M. - Okajima, T. - Ota, N. - Ozaki, M. - Paerels, F. - Paltani, S. - Petre, R. - Pinto, C. - Porter, F.S. - Pottschmidt, K. - Reynolds, C.S. - Safi-Harb, S. - Saito, S. - Sakai, K. - Sasaki, T. - Sato, G. - Sato, K. - Sato, R. - Sato, T. - Sawada, M. - Schartel, N. - Serlemtsos, P.J. - Seta, H. - Shidatsu, M. - Simionescu, A. - Smith, R.K. - Soong, Y. - Stawarz, L. - Sugawara, Y. - Sugita, S. - Szymkowiak, A. - Tajima, H. - Takahashi, H. - Takahashi, T. - Takeda, S. - Takei, Y. - Tamagawa, T. - Tamura, T. - Tanaka, T. - Tanaka, Y. - Tanaka, YT - Tashiro, MS - Tawara, Y. - Terada, Y. - Terashima, Y. - Tombesi, F. - Tomida, H. - Tsuboi, Y. - Tsujimoto, M. - Tsunemi, H. - Tsuru, TG - Uchida, H. - Uchiyama, H. - Uchiyama, Y. - Ueda, S. - Ueda, Y. - Uno, S. - Urry, CM - Ursino, E. - Watanabe, S. - Werner, Norbert - Wilkins, D.R. - Williams, B.J. - Yamada, S. - Yamaguchi, H. - Yamaoka, K. - Yamasaki, N.Y. - Yamauchi, M. - Yamauchi, S. - Yaqoob, T. - Yatsu, Y. - Yonetoku, D. - Zhuravleva, I. - Zoghbi, A. - Tominaga, N. - Moriya, TJ PY - 2018 TI - Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer JF - PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN VL - 70 IS - 2 SP - "14-1"-"14-17" EP - "14-1"-"14-17" PB - OXFORD UNIV PRESS SN - 00046264 KW - instrumentation: spectrographs KW - ISM: individual (Crab nebula) KW - ISM: supernova remnants KW - methods: observational UR - https://arxiv.org/pdf/1707.00054.pdf N2 - The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054 AD. When viewed as a supernova remnant (SNR), it has an anomalously low observed ejecta mass and kinetic energy for an Fe-core-collapse SN. Intensive searches have been made for a massive shell that solves this discrepancy, but none has been detected. An alternative idea is that SN 1054 is an electron-capture (EC) explosion with a lower explosion energy by an order of magnitude than Fe-core-collapse SNe. X-ray imaging searches were performed for the plasma emission from the shell in the Crab outskirts to set a stringent upper limit on the X-ray emitting mass. However, the extreme brightness of the source hampers access to its vicinity. We thus employed spectroscopic technique using the X-ray micro-calorimeter on board the Hitomi satellite. By exploiting its superb energy resolution, we set an upper limit for emission or absorption features from as yet undetected thermal plasma in the 2-12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data. By assembling these results, a new upper limit was obtained for the X-ray plasma mass of less than or similar to 1 M-circle dot for a wide range of assumed shell radius, size, and plasma temperature values both in and out of collisional equilibrium. To compare with the observation, we further performed hydrodynamic simulations of the Crab SNR for two SN models (Fe-core versus EC) under two SN environments (uniform interstellar medium versus progenitor wind). We found that the observed mass limit can be compatible with both SN models if the SN environment has a low density of less than or similar to 0.03 cm(-3) (Fe core) or less than or similar to 0.1 cm(-3) (EC) for the uniform density, or a progenitor wind density somewhat less than that provided by amass loss rate of 10(-5) M-circle dot yr(-1) at 20 km s(-1) for the wind environment. ER -
AHARONIAN, F.; H. AKAMATSU; F. AKIMOTO; S.W. ALLEN; L. ANGELINI; M. AUDARD; H. AWAKI; M. AXELSSON; A. BAMBA; M.W. BAUTZ; R. BLANDFORD; L.W. BRENNEMAN; GV. BROWN; E. BULBUL; EM. CACKETT; M. CHERNYAKOVA; MP CHIAO; P.S. COPPI; E. COSTANTINI; J. DE PLAA; C.P. DE VRIES; J.W. DEN HERDER; C. DONE; T. DOTANI; K. EBISAWA; ME. ECKART; T. ENOTO; Y. EZOE; A.C. FABIAN; C. FERRIGNO; A.R. FOSTER; R. FUJIMOTO; Y. FUKAZAWA; A. FURUZAWA; M. GALEAZZI; L.C. GALLO; P. GANDHI; M. GIUSTINI; A. GOLDWURM; Gu LY; M. GUAINAZZI; Y. HABA; K. HAGINO; K. HAMAGUCH; IM. HARRUS; I. HATSUKADE; K. HAYASHI; T. HAYASHI; K. HAYASHIDA; JS HIRAGA; A. HORNSCHEMEIER; A. HOSHINO; J.P. HUGHES; Y. ICHINOHE; R. IIZUKA; H. INOUE; Y. INOUE; M. ISHIDA; K. ISHIKAWA; Y. ISHISAKI; J. KAASTRA; T. KALLMAN; T. KAMAE; J. KATAOKA; S. KATSUDA; N. KAWAI; R.L. KELLEY; C.A. KILBOURNE; T. KITAGUCHI; S. KITAMOTO; T. KITAYAMA; T. KOHMURA; M. KOKUBUN; K. KOYAMA; S. KOYAMA; P. KRETSCHMAR; HA KRIMM; A. KUBOTA; H. KUNIEDA; P. LAURENT; SH. LEE; M.A. LEUTENEGGER; O. LIMOUSIN; M. LOEWENSTEIN; K.S. LONG; D. LUMB; G. MADEJSKI; Y. MAEDA; D. MAIER; K. MAKISHIMA; M. MARKEVITCH; H. MATSUMOTO; K. MATSUSHITA; D. MCCAMMON; B.R. MCNAMARA; M. MEHDIPOUR; E.D. MILLER; J.M. MILLER; S. MINESHIGE; K. MITSUDA; I. MITSUISHI; T. MIYAZAWA; T. MIZUNO; H. MORI; K. MORI; K. MUKAI; H. MURAKAMI; R.F. MUSHOTZKY; T. NAKAGAWA; H. NAKAJIMA; T. NAKAMORI; S. NAKASHIMA; K. NAKAZAWA; KK NOBUKAWA; M. NOBUKAWA; H. NODA; H. ODAKA; T. OHASHI; M. OHNO; T. OKAJIMA; N. OTA; M. OZAKI; F. PAERELS; S. PALTANI; R. PETRE; C. PINTO; F.S. PORTER; K. POTTSCHMIDT; C.S. REYNOLDS; S. SAFI-HARB; S. SAITO; K. SAKAI; T. SASAKI; G. SATO; K. SATO; R. SATO; T. SATO; M. SAWADA; N. SCHARTEL; P.J. SERLEMTSOS; H. SETA; M. SHIDATSU; A. SIMIONESCU; R.K. SMITH; Y. SOONG; L. STAWARZ; Y. SUGAWARA; S. SUGITA; A. SZYMKOWIAK; H. TAJIMA; H. TAKAHASHI; T. TAKAHASHI; S. TAKEDA; Y. TAKEI; T. TAMAGAWA; T. TAMURA; T. TANAKA; Y. TANAKA; YT TANAKA; MS TASHIRO; Y. TAWARA; Y. TERADA; Y. TERASHIMA; F. TOMBESI; H. TOMIDA; Y. TSUBOI; M. TSUJIMOTO; H. TSUNEMI; TG TSURU; H. UCHIDA; H. UCHIYAMA; Y. UCHIYAMA; S. UEDA; Y. UEDA; S. UNO; CM URRY; E. URSINO; S. WATANABE; Norbert WERNER; D.R. WILKINS; B.J. WILLIAMS; S. YAMADA; H. YAMAGUCHI; K. YAMAOKA; N.Y. YAMASAKI; M. YAMAUCHI; S. YAMAUCHI; T. YAQOOB; Y. YATSU; D. YONETOKU; I. ZHURAVLEVA; A. ZOGHBI; N. TOMINAGA a TJ MORIYA. Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer. \textit{PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN}. OXFORD: OXFORD UNIV PRESS, 2018, roč.~70, č.~2, s.~''14-1''-''14-17'', 17 s. ISSN~0004-6264. Dostupné z: https://doi.org/10.1093/pasj/psx072.