@article{
 title = {Hitomi X-ray observation of the pulsar wind nebula G21.5-0.9},
 type = {article},
 year = {2018},
 identifiers = {[object Object]},
 keywords = {ISM: individual objects(G21.5-0.9),ISM: supernovaremnants,pulsars: individual(PSR J1833-1034)},
 volume = {70},
 websites = {https://academic.oup.com/pasj/article/doi/10.1093/pasj/psy027/4961358},
 month = {6},
 publisher = {Oxford University Press},
 day = {1},
 id = {b6ab85e9-0166-349b-a295-d41f15d0b5cc},
 created = {2019-11-05T08:27:52.414Z},
 accessed = {2018-06-23},
 file_attached = {true},
 profile_id = {ec4888e4-cd9f-3ee0-90a1-39a024d1537d},
 last_modified = {2022-07-15T21:49:05.408Z},
 read = {true},
 starred = {false},
 authored = {true},
 confirmed = {true},
 hidden = {false},
 citation_key = {hitomi18j},
 source_type = {article},
 folder_uuids = {9989056f-58f0-4daf-a99f-4779f0cdd416,5a859072-32ae-4559-8859-863b99a8e32c},
 private_publication = {false},
 abstract = {We present results from the Hitomi X-ray observation of a young composite-type supernova remnant (SNR) G21.5-0.9, whose emission is dominated by the pulsar wind nebula (PWN) contribution. The X-ray spectra in the 0.8-80 keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager, and Hard X-ray Imager (HXI) show a significant break in the continuum as previously found with the NuSTAR observation. After taking into account all known emissions from the SNR other than the PWN itself, we find that the Hitomi spectra can be fitted with a broken power law with photon indices of 1 = 1.74 ± 0.02 and 2 = 2.14 ± 0.01 below and above the break at 7.1 ± 0.3 keV, which is significantly lower than the NuSTAR result (∼9.0 keV). The spectral break cannot be reproduced by time-dependent particle injection one-zone spectral energy distribution models, which strongly indicates that a more complex emission model is needed, as suggested by recent theoretical models. We also search for narrow emission or absorption lines with the SXS, and perform a timing analysis of PSR J1833-1034 with the HXI and the Soft Gamma-ray Detector. No significant pulsation is found from the pulsar. However, unexpectedly, narrow absorption line features are detected in the SXS data at 4.2345 keV and 9.296 keV with a significance of 3.65 s. While the origin of these features is not understood, their mere detection opens up a new field of research and was only possible with the high resolution, sensitivity, and ability to measure extended sources provided by an X-ray microcalorimeter.},
 bibtype = {article},
 author = {Aharonian, Felix and Akamatsu, Hiroki and Akimoto, Fumie and Allen, Steven W. and Angelini, Lorella and Audard, Marc and Awaki, Hisamitsu and Axelsson, Magnus and Bamba, Aya and Bautz, Marshall W. and Blandford, Roger and Brenneman, Laura W. and Brown, Gregory V. and Bulbul, Esra and Cackett, Edward M. and Chernyakova, Maria and Chiao, Meng P. and Coppi, Paolo S. and Costantini, Elisa and De Plaa, Jelle and De Vries, Cor P. and Den Herder, Jan Willem and Done, Chris and Dotani, Tadayasu and Ebisawa, Ken and Eckart, Megan E. and Enoto, Teruaki and Ezoe, Yuichiro and Fabian, Andrew C. and Ferrigno, Carlo and Foster, Adam R. and Fujimoto, Ryuichi and Fukazawa, Yasushi and Furuzawa, Akihiro and Galeazzi, Massimiliano and Gallo, Luigi C. and Gandhi, Poshak and Giustini, Margherita and Goldwurm, Andrea and Gu, Liyi and Guainazzi, Matteo and Haba, Yoshito and Hagino, Kouichi and Hamaguchi, Kenji and Harrus, Ilana M. and Hatsukade, Isamu and Hayashi, Katsuhiro and Hayashi, Takayuki and Hayashida, Kiyoshi and Hiraga, Junko S. and Hornschemeier, Ann and Hoshino, Akio and Hughes, John P. and Ichinohe, Yuto and Iizuka, Ryo and Inoue, Hajime and Inoue, Yoshiyuki and Ishida, Manabu and Ishikawa, Kumi and Ishisaki, Yoshitaka and Iwai, Masachika and Kaastra, Jelle and Kallman, Tim and Kamae, Tsuneyoshi and Kataoka, Jun and Katsuda, Satoru and Kawai, Nobuyuki and Kelley, Richard L. and Kilbourne, Caroline A. and Kitaguchi, Takao and Kitamoto, Shunji and Kitayama, Tetsu and Kohmura, Takayoshi and Kokubun, Motohide and Koyama, Katsuji and Koyama, Shu and Kretschmar, Peter and Krimm, Hans A. and Kubota, Aya and Kunieda, Hideyo and Laurent, Philippe and Lee, Shiu Hang and Leutenegger, Maurice A. and Limousin, Olivier and Loewenstein, Michael and Long, Knox S. and Lumb, David and Madejski, Greg and Maeda, Yoshitomo and Maier, Daniel and Makishima, Kazuo and Markevitch, Maxim and Matsumoto, Hironori and Matsushita, Kyoko and McCammon, Dan and McNamara, Brian R. and Mehdipour, Missagh and Miller, Eric D. and Miller, Jon M. and Mineshige, Shin and Mitsuda, Kazuhisa and Mitsuishi, Ikuyuki and Miyazawa, Takuya and Mizuno, Tsunefumi and Mori, Hideyuki and Mori, Koji and Mukai, Koji and Murakami, Hiroshi and Mushotzky, Richard F. and Nakagawa, Takao and Nakajima, Hiroshi and Nakamori, Takeshi and Nakashima, Shinya and Nakazawa, Kazuhiro and Nobukawa, Kumiko K. and Nobukawa, Masayoshi and Noda, Hirofumi and Odaka, Hirokazu and Ohashi, Takaya and Ohno, Masanori and Okajima, Takashi and Ota, Naomi and Ozaki, Masanobu and Paerels, Frits and Paltani, Stéphane and Petre, Robert and Pinto, Ciro and Porter, Frederick S. and Pottschmidt, Katja and Reynolds, Christopher S. and Safi-Harb, Samar and Saito, Shinya and Sakai, Kazuhiro and Sasaki, Toru and Sato, Goro and Sato, Kosuke and Sato, Rie and Sawada, Makoto and Schartel, Norbert and Serlemtsos, Peter J. and Seta, Hiromi and Shidatsu, Megumi and Simionescu, Aurora and Smith, Randall K. and Soong, Yang and Stawarz, Lukasz and Sugawara, Yasuharu and Sugita, Satoshi and Szymkowiak, Andrew and Tajima, Hiroyasu and Takahashi, Hiromitsu and Takahashi, Tadayuki and Takeda, Shin’Ichiro and Takei, Yoh and Tamagawa, Toru and Tamura, Takayuki and Tanaka, Takaaki and Tanaka, Yasuo and Tanaka, Yasuyuki T. and Tashiro, Makoto S. and Tawara, Yuzuru and Terada, Yukikatsu and Terashima, Yuichi and Tombesi, Francesco and Tomida, Hiroshi and Tsuboi, Yohko and Tsujimoto, Masahiro and Tsunemi, Hiroshi and Tsuru, Takeshi Go and Uchida, Hiroyuki and Uchiyama, Hideki and Uchiyama, Yasunobu and Ueda, Shutaro and Ueda, Yoshihiro and Uno, Shin’Ichiro and Urry, C. Megan and Ursino, Eugenio and Watanabe, Shin and Werner, Norbert and Wilkins, Dan R. and Williams, Brian J. and Yamada, Shinya and Yamaguchi, Hiroya and Yamaoka, Kazutaka and Yamasaki, Noriko Y. and Yamauchi, Makoto and Yamauchi, Shigeo and Yaqoob, Tahir and Yatsu, Yoichi and Yonetoku, Daisuke and Zhuravleva, Irina and Zoghbi, Abderahmen and Sato, Toshiki and Nakaniwa, Nozomu and Murakami, Hiroaki and Guest, Benson},
 journal = {Publications of the Astronomical Society of Japan},
 number = {3}
}

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The X-ray spectra in the 0.8-80 keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager, and Hard X-ray Imager (HXI) show a significant break in the continuum as previously found with the NuSTAR observation. After taking into account all known emissions from the SNR other than the PWN itself, we find that the Hitomi spectra can be fitted with a broken power law with photon indices of 1 = 1.74 ± 0.02 and 2 = 2.14 ± 0.01 below and above the break at 7.1 ± 0.3 keV, which is significantly lower than the NuSTAR result (∼9.0 keV). The spectral break cannot be reproduced by time-dependent particle injection one-zone spectral energy distribution models, which strongly indicates that a more complex emission model is needed, as suggested by recent theoretical models. We also search for narrow emission or absorption lines with the SXS, and perform a timing analysis of PSR J1833-1034 with the HXI and the Soft Gamma-ray Detector. No significant pulsation is found from the pulsar. However, unexpectedly, narrow absorption line features are detected in the SXS data at 4.2345 keV and 9.296 keV with a significance of 3.65 s. While the origin of these features is not understood, their mere detection opens up a new field of research and was only possible with the high resolution, sensitivity, and ability to measure extended sources provided by an X-ray microcalorimeter.","bibtype":"article","author":"Aharonian, Felix and Akamatsu, Hiroki and Akimoto, Fumie and Allen, Steven W. and Angelini, Lorella and Audard, Marc and Awaki, Hisamitsu and Axelsson, Magnus and Bamba, Aya and Bautz, Marshall W. and Blandford, Roger and Brenneman, Laura W. and Brown, Gregory V. and Bulbul, Esra and Cackett, Edward M. and Chernyakova, Maria and Chiao, Meng P. and Coppi, Paolo S. and Costantini, Elisa and De Plaa, Jelle and De Vries, Cor P. and Den Herder, Jan Willem and Done, Chris and Dotani, Tadayasu and Ebisawa, Ken and Eckart, Megan E. and Enoto, Teruaki and Ezoe, Yuichiro and Fabian, Andrew C. and Ferrigno, Carlo and Foster, Adam R. and Fujimoto, Ryuichi and Fukazawa, Yasushi and Furuzawa, Akihiro and Galeazzi, Massimiliano and Gallo, Luigi C. and Gandhi, Poshak and Giustini, Margherita and Goldwurm, Andrea and Gu, Liyi and Guainazzi, Matteo and Haba, Yoshito and Hagino, Kouichi and Hamaguchi, Kenji and Harrus, Ilana M. and Hatsukade, Isamu and Hayashi, Katsuhiro and Hayashi, Takayuki and Hayashida, Kiyoshi and Hiraga, Junko S. and Hornschemeier, Ann and Hoshino, Akio and Hughes, John P. and Ichinohe, Yuto and Iizuka, Ryo and Inoue, Hajime and Inoue, Yoshiyuki and Ishida, Manabu and Ishikawa, Kumi and Ishisaki, Yoshitaka and Iwai, Masachika and Kaastra, Jelle and Kallman, Tim and Kamae, Tsuneyoshi and Kataoka, Jun and Katsuda, Satoru and Kawai, Nobuyuki and Kelley, Richard L. and Kilbourne, Caroline A. and Kitaguchi, Takao and Kitamoto, Shunji and Kitayama, Tetsu and Kohmura, Takayoshi and Kokubun, Motohide and Koyama, Katsuji and Koyama, Shu and Kretschmar, Peter and Krimm, Hans A. and Kubota, Aya and Kunieda, Hideyo and Laurent, Philippe and Lee, Shiu Hang and Leutenegger, Maurice A. and Limousin, Olivier and Loewenstein, Michael and Long, Knox S. and Lumb, David and Madejski, Greg and Maeda, Yoshitomo and Maier, Daniel and Makishima, Kazuo and Markevitch, Maxim and Matsumoto, Hironori and Matsushita, Kyoko and McCammon, Dan and McNamara, Brian R. and Mehdipour, Missagh and Miller, Eric D. and Miller, Jon M. and Mineshige, Shin and Mitsuda, Kazuhisa and Mitsuishi, Ikuyuki and Miyazawa, Takuya and Mizuno, Tsunefumi and Mori, Hideyuki and Mori, Koji and Mukai, Koji and Murakami, Hiroshi and Mushotzky, Richard F. and Nakagawa, Takao and Nakajima, Hiroshi and Nakamori, Takeshi and Nakashima, Shinya and Nakazawa, Kazuhiro and Nobukawa, Kumiko K. and Nobukawa, Masayoshi and Noda, Hirofumi and Odaka, Hirokazu and Ohashi, Takaya and Ohno, Masanori and Okajima, Takashi and Ota, Naomi and Ozaki, Masanobu and Paerels, Frits and Paltani, Stéphane and Petre, Robert and Pinto, Ciro and Porter, Frederick S. and Pottschmidt, Katja and Reynolds, Christopher S. and Safi-Harb, Samar and Saito, Shinya and Sakai, Kazuhiro and Sasaki, Toru and Sato, Goro and Sato, Kosuke and Sato, Rie and Sawada, Makoto and Schartel, Norbert and Serlemtsos, Peter J. and Seta, Hiromi and Shidatsu, Megumi and Simionescu, Aurora and Smith, Randall K. and Soong, Yang and Stawarz, Lukasz and Sugawara, Yasuharu and Sugita, Satoshi and Szymkowiak, Andrew and Tajima, Hiroyasu and Takahashi, Hiromitsu and Takahashi, Tadayuki and Takeda, Shin’Ichiro and Takei, Yoh and Tamagawa, Toru and Tamura, Takayuki and Tanaka, Takaaki and Tanaka, Yasuo and Tanaka, Yasuyuki T. and Tashiro, Makoto S. and Tawara, Yuzuru and Terada, Yukikatsu and Terashima, Yuichi and Tombesi, Francesco and Tomida, Hiroshi and Tsuboi, Yohko and Tsujimoto, Masahiro and Tsunemi, Hiroshi and Tsuru, Takeshi Go and Uchida, Hiroyuki and Uchiyama, Hideki and Uchiyama, Yasunobu and Ueda, Shutaro and Ueda, Yoshihiro and Uno, Shin’Ichiro and Urry, C. Megan and Ursino, Eugenio and Watanabe, Shin and Werner, Norbert and Wilkins, Dan R. and Williams, Brian J. and Yamada, Shinya and Yamaguchi, Hiroya and Yamaoka, Kazutaka and Yamasaki, Noriko Y. and Yamauchi, Makoto and Yamauchi, Shigeo and Yaqoob, Tahir and Yatsu, Yoichi and Yonetoku, Daisuke and Zhuravleva, Irina and Zoghbi, Abderahmen and Sato, Toshiki and Nakaniwa, Nozomu and Murakami, Hiroaki and Guest, Benson","journal":"Publications of the Astronomical Society of Japan","number":"3","bibtex":"@article{\n title = {Hitomi X-ray observation of the pulsar wind nebula G21.5-0.9},\n type = {article},\n year = {2018},\n identifiers = {[object Object]},\n keywords = {ISM: individual objects(G21.5-0.9),ISM: supernovaremnants,pulsars: individual(PSR J1833-1034)},\n volume = {70},\n websites = {https://academic.oup.com/pasj/article/doi/10.1093/pasj/psy027/4961358},\n month = {6},\n publisher = {Oxford University Press},\n day = {1},\n id = {b6ab85e9-0166-349b-a295-d41f15d0b5cc},\n created = {2019-11-05T08:27:52.414Z},\n accessed = {2018-06-23},\n file_attached = {true},\n profile_id = {ec4888e4-cd9f-3ee0-90a1-39a024d1537d},\n last_modified = {2022-07-15T21:49:05.408Z},\n read = {true},\n starred = {false},\n authored = {true},\n confirmed = {true},\n hidden = {false},\n citation_key = {hitomi18j},\n source_type = {article},\n folder_uuids = {9989056f-58f0-4daf-a99f-4779f0cdd416,5a859072-32ae-4559-8859-863b99a8e32c},\n private_publication = {false},\n abstract = {We present results from the Hitomi X-ray observation of a young composite-type supernova remnant (SNR) G21.5-0.9, whose emission is dominated by the pulsar wind nebula (PWN) contribution. The X-ray spectra in the 0.8-80 keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager, and Hard X-ray Imager (HXI) show a significant break in the continuum as previously found with the NuSTAR observation. After taking into account all known emissions from the SNR other than the PWN itself, we find that the Hitomi spectra can be fitted with a broken power law with photon indices of 1 = 1.74 ± 0.02 and 2 = 2.14 ± 0.01 below and above the break at 7.1 ± 0.3 keV, which is significantly lower than the NuSTAR result (∼9.0 keV). The spectral break cannot be reproduced by time-dependent particle injection one-zone spectral energy distribution models, which strongly indicates that a more complex emission model is needed, as suggested by recent theoretical models. We also search for narrow emission or absorption lines with the SXS, and perform a timing analysis of PSR J1833-1034 with the HXI and the Soft Gamma-ray Detector. No significant pulsation is found from the pulsar. However, unexpectedly, narrow absorption line features are detected in the SXS data at 4.2345 keV and 9.296 keV with a significance of 3.65 s. While the origin of these features is not understood, their mere detection opens up a new field of research and was only possible with the high resolution, sensitivity, and ability to measure extended sources provided by an X-ray microcalorimeter.},\n bibtype = {article},\n author = {Aharonian, Felix and Akamatsu, Hiroki and Akimoto, Fumie and Allen, Steven W. and Angelini, Lorella and Audard, Marc and Awaki, Hisamitsu and Axelsson, Magnus and Bamba, Aya and Bautz, Marshall W. and Blandford, Roger and Brenneman, Laura W. and Brown, Gregory V. and Bulbul, Esra and Cackett, Edward M. and Chernyakova, Maria and Chiao, Meng P. and Coppi, Paolo S. and Costantini, Elisa and De Plaa, Jelle and De Vries, Cor P. and Den Herder, Jan Willem and Done, Chris and Dotani, Tadayasu and Ebisawa, Ken and Eckart, Megan E. and Enoto, Teruaki and Ezoe, Yuichiro and Fabian, Andrew C. and Ferrigno, Carlo and Foster, Adam R. and Fujimoto, Ryuichi and Fukazawa, Yasushi and Furuzawa, Akihiro and Galeazzi, Massimiliano and Gallo, Luigi C. and Gandhi, Poshak and Giustini, Margherita and Goldwurm, Andrea and Gu, Liyi and Guainazzi, Matteo and Haba, Yoshito and Hagino, Kouichi and Hamaguchi, Kenji and Harrus, Ilana M. and Hatsukade, Isamu and Hayashi, Katsuhiro and Hayashi, Takayuki and Hayashida, Kiyoshi and Hiraga, Junko S. and Hornschemeier, Ann and Hoshino, Akio and Hughes, John P. and Ichinohe, Yuto and Iizuka, Ryo and Inoue, Hajime and Inoue, Yoshiyuki and Ishida, Manabu and Ishikawa, Kumi and Ishisaki, Yoshitaka and Iwai, Masachika and Kaastra, Jelle and Kallman, Tim and Kamae, Tsuneyoshi and Kataoka, Jun and Katsuda, Satoru and Kawai, Nobuyuki and Kelley, Richard L. and Kilbourne, Caroline A. and Kitaguchi, Takao and Kitamoto, Shunji and Kitayama, Tetsu and Kohmura, Takayoshi and Kokubun, Motohide and Koyama, Katsuji and Koyama, Shu and Kretschmar, Peter and Krimm, Hans A. and Kubota, Aya and Kunieda, Hideyo and Laurent, Philippe and Lee, Shiu Hang and Leutenegger, Maurice A. and Limousin, Olivier and Loewenstein, Michael and Long, Knox S. and Lumb, David and Madejski, Greg and Maeda, Yoshitomo and Maier, Daniel and Makishima, Kazuo and Markevitch, Maxim and Matsumoto, Hironori and Matsushita, Kyoko and McCammon, Dan and McNamara, Brian R. and Mehdipour, Missagh and Miller, Eric D. and Miller, Jon M. and Mineshige, Shin and Mitsuda, Kazuhisa and Mitsuishi, Ikuyuki and Miyazawa, Takuya and Mizuno, Tsunefumi and Mori, Hideyuki and Mori, Koji and Mukai, Koji and Murakami, Hiroshi and Mushotzky, Richard F. and Nakagawa, Takao and Nakajima, Hiroshi and Nakamori, Takeshi and Nakashima, Shinya and Nakazawa, Kazuhiro and Nobukawa, Kumiko K. and Nobukawa, Masayoshi and Noda, Hirofumi and Odaka, Hirokazu and Ohashi, Takaya and Ohno, Masanori and Okajima, Takashi and Ota, Naomi and Ozaki, Masanobu and Paerels, Frits and Paltani, Stéphane and Petre, Robert and Pinto, Ciro and Porter, Frederick S. and Pottschmidt, Katja and Reynolds, Christopher S. and Safi-Harb, Samar and Saito, Shinya and Sakai, Kazuhiro and Sasaki, Toru and Sato, Goro and Sato, Kosuke and Sato, Rie and Sawada, Makoto and Schartel, Norbert and Serlemtsos, Peter J. and Seta, Hiromi and Shidatsu, Megumi and Simionescu, Aurora and Smith, Randall K. and Soong, Yang and Stawarz, Lukasz and Sugawara, Yasuharu and Sugita, Satoshi and Szymkowiak, Andrew and Tajima, Hiroyasu and Takahashi, Hiromitsu and Takahashi, Tadayuki and Takeda, Shin’Ichiro and Takei, Yoh and Tamagawa, Toru and Tamura, Takayuki and Tanaka, Takaaki and Tanaka, Yasuo and Tanaka, Yasuyuki T. and Tashiro, Makoto S. and Tawara, Yuzuru and Terada, Yukikatsu and Terashima, Yuichi and Tombesi, Francesco and Tomida, Hiroshi and Tsuboi, Yohko and Tsujimoto, Masahiro and Tsunemi, Hiroshi and Tsuru, Takeshi Go and Uchida, Hiroyuki and Uchiyama, Hideki and Uchiyama, Yasunobu and Ueda, Shutaro and Ueda, Yoshihiro and Uno, Shin’Ichiro and Urry, C. Megan and Ursino, Eugenio and Watanabe, Shin and Werner, Norbert and Wilkins, Dan R. and Williams, Brian J. and Yamada, Shinya and Yamaguchi, Hiroya and Yamaoka, Kazutaka and Yamasaki, Noriko Y. and Yamauchi, Makoto and Yamauchi, Shigeo and Yaqoob, Tahir and Yatsu, Yoichi and Yonetoku, Daisuke and Zhuravleva, Irina and Zoghbi, Abderahmen and Sato, Toshiki and Nakaniwa, Nozomu and Murakami, Hiroaki and Guest, Benson},\n journal = {Publications of the Astronomical Society of Japan},\n number = {3}\n}","author_short":["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, G., V.","Bulbul, E.","Cackett, E., M.","Chernyakova, M.","Chiao, M., P.","Coppi, P., S.","Costantini, E.","De Plaa, J.","De Vries, C., P.","Den Herder, J., W.","Done, C.","Dotani, T.","Ebisawa, K.","Eckart, M., E.","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.","Gu, L.","Guainazzi, M.","Haba, Y.","Hagino, K.","Hamaguchi, K.","Harrus, I., M.","Hatsukade, I.","Hayashi, K.","Hayashi, T.","Hayashida, K.","Hiraga, J., S.","Hornschemeier, A.","Hoshino, A.","Hughes, J., P.","Ichinohe, Y.","Iizuka, R.","Inoue, H.","Inoue, Y.","Ishida, M.","Ishikawa, K.","Ishisaki, Y.","Iwai, M.","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, H., A.","Kubota, A.","Kunieda, H.","Laurent, P.","Lee, S., H.","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, K., K.","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.","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, Y., T.","Tashiro, M., S.","Tawara, Y.","Terada, Y.","Terashima, Y.","Tombesi, F.","Tomida, H.","Tsuboi, Y.","Tsujimoto, M.","Tsunemi, H.","Tsuru, T., G.","Uchida, H.","Uchiyama, H.","Uchiyama, Y.","Ueda, S.","Ueda, Y.","Uno, S.","Urry, C., M.","Ursino, E.","Watanabe, S.","Werner, N.","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.","Sato, T.","Nakaniwa, N.","Murakami, H.","Guest, B."],"urls":{"Website":"https://academic.oup.com/pasj/article/doi/10.1093/pasj/psy027/4961358"},"biburl":"https://bibbase.org/service/mendeley/ec4888e4-cd9f-3ee0-90a1-39a024d1537d","bibbaseid":"aharonian-akamatsu-akimoto-allen-angelini-audard-awaki-axelsson-etal-hitomixrayobservationofthepulsarwindnebulag21509-2018","role":"author","keyword":["ISM: individual objects(G21.5-0.9)","ISM: supernovaremnants","pulsars: individual(PSR J1833-1034)"],"metadata":{"authorlinks":{}},"html":""},"bibtype":"article","biburl":"https://bibbase.org/service/mendeley/ec4888e4-cd9f-3ee0-90a1-39a024d1537d","dataSources":["RmgzPftd92tGag9se"],"keywords":["ism: individual objects(g21.5-0.9)","ism: supernovaremnants","pulsars: individual(psr j1833-1034)"],"search_terms":["hitomi","ray","observation","pulsar","wind","nebula","g21","aharonian","akamatsu","akimoto","allen","angelini","audard","awaki","axelsson","bamba","bautz","blandford","brenneman","brown","bulbul","cackett","chernyakova","chiao","coppi","costantini","de plaa","de vries","den 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X-ray observation of the pulsar wind nebula G21.5-0.9","year":2018}