抄録
The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054AD. 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 2-12keV 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 < 1 M⊙ 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 < 0.03 cm-3 (Fe core) or < 0.1 cm-3 (EC) for the uniform density, or a progenitor wind density somewhat less than that provided by a mass loss rate of 10-5M⊙ yr-1 at 20 km s-1for the wind environment.
| 本文言語 | English |
|---|---|
| 論文番号 | psx072 |
| ジャーナル | Publications of the Astronomical Society of Japan |
| 巻 | 70 |
| 号 | 2 |
| DOI | |
| 出版ステータス | Published - 2018 3月 1 |
ASJC Scopus subject areas
- 天文学と天体物理学
- 宇宙惑星科学
フィンガープリント
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In: Publications of the Astronomical Society of Japan, Vol. 70, No. 2, psx072, 01.03.2018.
研究成果: Article › 査読
}
TY - JOUR
T1 - Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer
AU - Moriya, Takashi J.
AU - Aharonian, Felix
AU - Akamatsu, Hiroki
AU - Akimoto, Fumie
AU - Allen, Steven W.
AU - Angelini, Lorella
AU - Audard, Marc
AU - Awaki, Hisamitsu
AU - Axelsson, Magnus
AU - Bamba, Aya
AU - Bautz, Marshall W.
AU - Blandford, Roger
AU - Brenneman, Laura W.
AU - Brown, Gregory V.
AU - Bulbul, Esra
AU - Cackett, Edward M.
AU - Chernyakova, Maria
AU - Chiao, Meng P.
AU - Coppi, Paolo S.
AU - Costantini, Elisa
AU - De Plaa, Jelle
AU - De Vries, Cor P.
AU - Den Herder, Jan Willem
AU - Done, Chris
AU - Dotani, Tadayasu
AU - Ebisawa, Ken
AU - Eckart, Megan E.
AU - Enoto, Teruaki
AU - Ezoe, Yuichiro
AU - Fabian, Andrew C.
AU - Ferrigno, Carlo
AU - Foster, Adam R.
AU - Fujimoto, Ryuichi
AU - Fukazawa, Yasushi
AU - Furuzawa, Akihiro
AU - Galeazzi, Massimiliano
AU - Gallo, Luigi C.
AU - Gandhi, Poshak
AU - Giustini, Margherita
AU - Goldwurm, Andrea
AU - Gu, Liyi
AU - Guainazzi, Matteo
AU - Haba, Yoshito
AU - Hagino, Kouichi
AU - Hamaguchi, Kenji
AU - Harrus, Ilana M.
AU - Hatsukade, Isamu
AU - Hayashi, Katsuhiro
AU - Hayashi, Takayuki
AU - Hayashida, Kiyoshi
AU - Hiraga, Junko S.
AU - Hornschemeier, Ann
AU - Hoshino, Akio
AU - Hughes, John P.
AU - Ichinohe, Yuto
AU - Iizuka, Ryo
AU - Inoue, Hajime
AU - Inoue, Yoshiyuki
AU - Ishida, Manabu
AU - Ishikawa, Kumi
AU - Ishisaki, Yoshitaka
AU - Kaastra, Jelle
AU - Kallman, Tim
AU - Kamae, Tsuneyoshi
AU - Kataoka, Jun
AU - Katsuda, Satoru
AU - Kawai, Nobuyuki
AU - Kelley, Richard L.
AU - Kilbourne, Caroline A.
AU - Kitaguchi, Takao
AU - Kitamoto, Shunji
AU - Kitayama, Tetsu
AU - Kohmura, Takayoshi
AU - Kokubun, Motohide
AU - Koyama, Katsuji
AU - Koyama, Shu
AU - Kretschmar, Peter
AU - Krimm, Hans A.
AU - Kubota, Aya
AU - Kunieda, Hideyo
AU - Laurent, Philippe
AU - Lee, Shiu Hang
AU - Leutenegger, Maurice A.
AU - Limousin, Olivier
AU - Loewenstein, Michael
AU - Long, Knox S.
AU - Lumb, David
AU - Madejski, Greg
AU - Maeda, Yoshitomo
AU - Maier, Daniel
AU - Makishima, Kazuo
AU - Markevitch, Maxim
AU - Matsumoto, Hironori
AU - Matsushita, Kyoko
AU - Mccammon, Dan
AU - Mcnamara, Brian R.
AU - Mehdipour, Missagh
AU - Miller, Eric D.
AU - Miller, Jon M.
AU - Mineshige, Shin
AU - Mitsuda, Kazuhisa
AU - Mitsuishi, Ikuyuki
AU - Miyazawa, Takuya
AU - Mizuno, Tsunefumi
AU - Mori, Hideyuki
AU - Mori, Koji
AU - Mukai, Koji
AU - Murakami, Hiroshi
AU - Mushotzky, Richard F.
AU - Nakagawa, Takao
AU - Nakajima, Hiroshi
AU - Nakamori, Takeshi
AU - Nakashima, Shinya
AU - Nakazawa, Kazuhiro
AU - Nobukawa, Kumiko K.
AU - Nobukawa, Masayoshi
AU - Noda, Hirofumi
AU - Odaka, Hirokazu
AU - Ohashi, Takaya
AU - Ohno, Masanori
AU - Okajima, Takashi
AU - Ota, Naomi
AU - Ozaki, Masanobu
AU - Paerels, Frits
AU - Paltani, Stéphane
AU - Petre, Robert
AU - Pinto, Ciro
AU - Porter, Frederick S.
AU - Pottschmidt, Katja
AU - Reynolds, Christopher S.
AU - Safi-Harb, Samar
AU - Saito, Shinya
AU - Sakai, Kazuhiro
AU - Sasaki, Toru
AU - Sato, Goro
AU - Sato, Kosuke
AU - Sato, Rie
AU - Sato, Toshiki
AU - Sawada, Makoto
AU - Schartel, Norbert
AU - Serlemtsos, Peter J.
AU - Seta, Hiromi
AU - Shidatsu, Megumi
AU - Simionescu, Aurora
AU - Smith, Randall K.
AU - Soong, Yang
AU - Stawarz, Łukasz
AU - Sugawara, Yasuharu
AU - Sugita, Satoshi
AU - Szymkowiak, Andrew
AU - Tajima, Hiroyasu
AU - Takahashi, Hiromitsu
AU - Takahashi, Tadayuki
AU - Takeda, Shin'ichiro
AU - Takei, Yoh
AU - Tamagawa, Toru
AU - Tamura, Takayuki
AU - Tanaka, Takaaki
AU - Tanaka, Yasuo
AU - Tanaka, Yasuyuki T.
AU - Tashiro, Makoto S.
AU - Tawara, Yuzuru
AU - Terada, Yukikatsu
AU - Terashima, Yuichi
AU - Tombesi, Francesco
AU - Tomida, Hiroshi
AU - Tsuboi, Yohko
AU - Tsujimoto, Masahiro
AU - Tsunemi, Hiroshi
AU - Tsuru, Takeshi Go
AU - Uchida, Hiroyuki
AU - Uchiyama, Hideki
AU - Uchiyama, Yasunobu
AU - Ueda, Shutaro
AU - Ueda, Yoshihiro
AU - Uno, Shin'ichiro
AU - Urry, C. Megan
AU - Ursino, Eugenio
AU - Watanabe, Shin
AU - Werner, Norbert
AU - Wilkins, Dan R.
AU - Williams, Brian J.
AU - Yamada, Shinya
AU - Yamaguchi, Hiroya
AU - Yamaoka, Kazutaka
AU - Yamasaki, Noriko Y.
AU - Yamauchi, Makoto
AU - Yamauchi, Shigeo
AU - Yaqoob, Tahir
AU - Yatsu, Yoichi
AU - Yonetoku, Daisuke
AU - Zhuravleva, Irina
AU - Zoghbi, Abderahmen
AU - Tominaga, Nozomu
N1 - Funding Information: We acknowledge the support of the JSPS Core-to-Core Program. We thank all the JAXA members who have contributed to the ASTRO-H (Hitomi) project. All U.S. members gratefully acknowledge support through the NASA Science Mission Directorate. Stanford and SLAC members acknowledge support via the DoE contract to SLAC National Accelerator Laboratory DE-AC3-76SF00515. Part of this work was performed under Funding Information: the auspices of the U.S. DoE by LLNL under Contract DE-AC52-07NA27344. Support from the European Space Agency is gratefully acknowledged. French members acknowledge support from CNES, the Centre National d’Études Spatiales. SRON is supported by NWO, the Netherlands Organization for Scientific Research. The Swiss team acknowledges the support of the Swiss Secretariat for Education, Research and Innovation (SERI). The Canadian Space Agency is acknowledged for the support of the Canadian members. We acknowledge support from JSPS/MEXT KAKENHI grant numbers JP15H00773, JP15H00785, JP15H02070, JP15H02090, JP15H03639, JP15H03641, JP15H03642, JP15H05438, JP15H06896, JP15K05107, JP15K17610, JP15K17657, JP16H00949, JP16H03983, JP16H06342, JP16J02333, JP16K05295, JP16K05296, JP16K05300, JP16K05309, JP16K13787, JP16K17667, JP16K17672, JP16K17673, JP17H02864, JP17K05393, JP21659292, JP23340055, JP23340071, JP23540280, JP24105007, JP24540232, JP25105516, JP25109004, JP25247028, JP25287042, JP25400236, JP25800119, JP26109506, JP26220703, JP26400228, JP26610047, and JP26800102. The following NASA grants are acknowledged: NNX15AC76G, NNX15AE16G, NNX15AK71G, NNX15AU54G, NNX15AW94G, and NNG15PP48P to Eureka Scientific. This work was partly supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan, and also by the Research Fellowship of JSPS for Young Scientists. H. Akamatsu acknowledges the support of NWO via a Veni grant. C. Done acknowledges STFC funding under grant ST/L00075X/1. A. Fabian and C. Pinto acknowledge ERC Advanced Grant 340442. P. Gandhi acknowledges a JAXA International Top Young Fellowship and UK Science and Technology Funding Council (STFC) grant ST/J003697/2. Y. Ichinohe, K. Nobukawa, H. Seta, and T. Sato are supported by the Research Fellow of JSPS for Young Scientists. N. Kawai is supported by the Grant-in-Aid for Scientific Research on Innovative Areas “New Developments in Astrophysics Through Multi-Messenger Observations of Gravitational Wave Sources”. S. Kitamoto is partially supported by the MEXT Supported Program for the Strategic Research Foundation at Private Universities, 2014– 2018. B. McNamara and S. Safi-Harb acknowledge support from NSERC. T. Dotani, T. Takahashi, T. Tamagawa, M. Tsujimoto, and Y. Uchiyama acknowledge support from the Grant-in-Aid for Scientific Research on Innovative Areas “Nuclear Matter in Neutron Stars Investigated by Experiments and Astronomical Observations”. N. Werner is supported by the Lendület LP2016-11 grant from the Hungarian Academy of Sciences. D. Wilkins is supported by NASA through Einstein Fellowship grant number PF6-170160, awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Funding Information: We appreciate all the people who contributed to the SXS, which made this work possible. We also thank Toru Misawa at Shinshu University for discussing the CIV feature. We acknowledge the support of the JSPS Core-to-Core Program. We thank all the JAXA members who have contributed to the ASTRO-H (Hitomi) project. All U.S. members gratefully acknowledge support through the NASA Science Mission Directorate. Stanford and SLAC members acknowledge support via the DoE contract to SLAC National Accelerator Laboratory DE-AC3-76SF00515. Part of this work was performed under the auspices of the U.S. DoE by LLNL under Contract DE-AC52-07NA27344. Support from the European Space Agency is gratefully acknowledged. French members acknowledge support from CNES, the Centre National d'?tudes Spatiales. SRON is supported by NWO, the Netherlands Organization for Scientific Research. The Swiss team acknowledges the support of the Swiss Secretariat for Education, Research and Innovation (SERI). The Canadian Space Agency is acknowledged for the support of the Canadian members. We acknowledge support from JSPS/MEXT KAKENHI grant numbers JP15H00773, JP15H00785, JP15H02070, JP15H02090, JP15H03639, JP15H03641, JP15H03642, JP15H05438, JP15H06896, JP15K05107, JP15K17610, JP15K17657, JP16H00949, JP16H03983, JP16H06342, JP16J02333, JP16K05295, JP16K05296, JP16K05300, JP16K05309, JP16K13787, JP16K17667, JP16K17672, JP16K17673, JP17H02864, JP17K05393, JP21659292, JP23340055, JP23340071, JP23540280, JP24105007, JP24540232, JP25105516, JP25109004, JP25247028, JP25287042, JP25400236, JP25800119, JP26109506, JP26220703, JP26400228, JP26610047, and JP26800102. The following NASA grants are acknowledged: NNX15AC76G, NNX15AE16G, NNX15AK71G, NNX15AU54G, NNX15AW94G, and NNG15PP48P to Eureka Scientific. This work was partly supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan, and also by the Research Fellowship of JSPS for Young Scientists. H. Akamatsu acknowledges the support of NWO via a Veni grant. C. Done acknowledges STFC funding under grant ST/L00075X/1. A. Fabian and C. Pinto acknowledge ERC Advanced Grant 340442. P. Gandhi acknowledges a JAXA International Top Young Fellowship and UK Science and Technology Funding Council (STFC) grant ST/J003697/2. Y. Ichinohe, K. Nobukawa, H. Seta, and T. Sato are supported by the Research Fellow of JSPS for Young Scientists. N. Kawai is supported by the Grant-in-Aid for Scientific Research on Innovative Areas "New Developments in Astrophysics Through Multi-Messenger Observations of Gravitational Wave Sources". S. Kitamoto is partially supported by the MEXT Supported Program for the Strategic Research Foundation at Private Universities, 2014-2018. B. McNamara and S. Safi-Harb acknowledge support from NSERC. T. Dotani, T. Takahashi, T. Tamagawa, M. Tsujimoto, and Y. Uchiyama acknowledge support from the Grant-in-Aid for Scientific Research on Innovative Areas "Nuclear Matter in Neutron Stars Investigated by Experiments and Astronomical Observations". N. Werner is supported by the Lend?let LP2016-11 grant from the Hungarian Academy of Sciences. D. Wilkins is supported by NASA through Einstein Fellowship grant number PF6-170160, awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We acknowledge the contributions of many companies, including, in particular, NEC, Mitsubishi Heavy Industries, Sumitomo Heavy Industries, and Japan Aviation Electronics Industry. Finally, we acknowledge strong support from the following engineers. JAXA/ISAS: Chris Baluta, Nobutaka Bando, Atsushi Harayama, Kazuyuki Hirose, Kosei Ishimura, Naoko Iwata, Taro Kawano, Shigeo Kawasaki, Kenji Minesugi, Chikara Natsukari, Hiroyuki Ogawa, Mina Ogawa, Masayuki Ohta, Tsuyoshi Okazaki, Shin-ichiro Sakai, Yasuko Shibano, Maki Shida, Takanobu Shimada, Atsushi Wada, Takahiro Yamada; JAXA/TKSC: Atsushi Okamoto, Yoichi Sato, Keisuke Shinozaki, Hiroyuki Sugita; Chubu Univ.: Yoshiharu Namba; Ehime Univ.: Keiji Ogi; Kochi Univ. of Technology: Tatsuro Kosaka; Miyazaki Univ.: Yusuke Nishioka; Nagoya Univ.: Housei Nagano; NASA/GSFC: Thomas Bialas, Kevin Boyce, Edgar Canavan, Michael DiPirro, Mark Kimball, Candace Masters, Daniel McGuinness, Joseph Miko, Theodore Muench, James Pontius, Peter Shirron, Cynthia Simmons, Gary Sneiderman, Tomomi Watanabe; ADNET Systems: Michael Witthoeft, Kristin Rutkowski, Robert S. Hill, Joseph Eggen; Wyle Information Systems: Andrew Sargent, Michael Dutka; Noqsi Aerospace Ltd: John Doty; Stanford Univ./KIPAC: Makoto Asai, Kirk Gilmore; ESA (Netherlands): Chris Jewell; SRON: Daniel Haas, Martin Frericks, Philippe Laubert, Paul Lowes; Univ. of Geneva: Philipp Azzarello; CSA: Alex Koujelev, Franco Moroso. Publisher Copyright: © The Author(s) 2017. Published by Oxford University Press on behalf of the Astronomical Society of Japan. All rights reserved.
PY - 2018/3/1
Y1 - 2018/3/1
N2 - The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054AD. 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 2-12keV 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 < 1 M⊙ 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 < 0.03 cm-3 (Fe core) or < 0.1 cm-3 (EC) for the uniform density, or a progenitor wind density somewhat less than that provided by a mass loss rate of 10-5M⊙ yr-1 at 20 km s-1for the wind environment.
AB - The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054AD. 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 2-12keV 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 < 1 M⊙ 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 < 0.03 cm-3 (Fe core) or < 0.1 cm-3 (EC) for the uniform density, or a progenitor wind density somewhat less than that provided by a mass loss rate of 10-5M⊙ yr-1 at 20 km s-1for the wind environment.
KW - ISM: individual (Crab nebula)-ISM: supernova remnants
KW - Instrumentation: spectrographs
KW - Methods: observational
UR - http://www.scopus.com/inward/record.url?scp=85058343250&partnerID=8YFLogxK
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U2 - 10.1093/pasj/psx072
DO - 10.1093/pasj/psx072
M3 - Article
AN - SCOPUS:85058343250
SN - 0004-6264
VL - 70
JO - Publication of the Astronomical Society of Japan
JF - Publication of the Astronomical Society of Japan
IS - 2
M1 - psx072
ER -