@article{
 title = {Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi},
 type = {article},
 year = {2018},
 identifiers = {[object Object]},
 keywords = {Binaries: general,Stars: individual (IGR J16318-4848),X-rays: binaries},
 volume = {70},
 websites = {https://academic.oup.com/pasj/article/doi/10.1093/pasj/psx154/4969728},
 month = {3},
 publisher = {Oxford University Press},
 day = {1},
 id = {be53b7b5-8927-3fd6-b8ef-d4b9a66f6a15},
 created = {2018-06-23T07:27:33.792Z},
 accessed = {2018-06-23},
 file_attached = {true},
 profile_id = {ec4888e4-cd9f-3ee0-90a1-39a024d1537d},
 last_modified = {2022-07-15T21:49:30.000Z},
 read = {true},
 starred = {false},
 authored = {true},
 confirmed = {true},
 hidden = {false},
 citation_key = {hitomi18i},
 folder_uuids = {9989056f-58f0-4daf-a99f-4779f0cdd416,5a859072-32ae-4559-8859-863b99a8e32c},
 private_publication = {false},
 abstract = {We report on a Hitomi observation of IGRJ16318-4848, a high-mass X-ray binary system with an extremely strong absorption of NH ∼ 1024cm 2. Previous X-ray studies revealed that its spectrum is dominated by strong fluorescence lines of Fe as well as continuum emission lines. For physical and geometrical insight into the nature of the reprocessing material, we utilized the high spectroscopic resolving power of the X-ray microcalorimeter (the soft X-ray spectrometer: SXS) and the wide-band sensitivity by the soft and hard X-ray imagers (SXI and HXI) aboard Hitomi. Even though the photon counts are limited due to unintended off-axis pointing, the SXS spectrum resolves Fe Kα1 and Kα2 lines and puts strong constraints on the line centroid and line width. The line width corresponds to a velocity of 160+-37000 km s-1. This represents the most accurate, and smallest, width measurement of this line made so far from the any X-ray binary, much less than the Doppler broadening and Doppler shift expected from speeds that are characteristic of similar systems. Combined with the K-shell edge energy measured by the SXI and HXI spectra, the ionization state of Fe is estimated to be in the range of Fe I-IV. Considering the estimated ionization parameter and the distance between the X-ray source and the absorber, the density and thickness of the materials are estimated. The extraordinarily strong absorption and the absence of a Compton shoulder component have been confirmed. These characteristics suggest reprocessing materials that are distributed in a narrow solid angle or scattering, primarily by warm free electrons or neutral hydrogen. This measurement was achieved using the SXS detection of 19 photons. It provides strong motivation for follow-up observations of this and other X-ray binaries using the X-ray Astrophysics Recovery Mission and other comparable future instruments.},
 bibtype = {article},
 author = {Alle, Steven W. and 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 O. 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, Łukasz and Sugawara, Yasuharu and Sugita, Satoshi and Szymkowiak, Andrew and Tajima, Hiroyasu and Takahashi, Hiromitsu and Takahashi, Tadayuki and Takeda, Shiníchiro 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 Suru, Takeshi Got and Uchida, Hiroyuki and Uchiyama, Hideki and Uchiyama, Yasunobu and Ueda, Shutaro and Ueda, Yoshihiro and Uno, Shiníchiro 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 Nakaniwa, Nozomi},
 journal = {Publications of the Astronomical Society of Japan},
 number = {2}
}

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Previous X-ray studies revealed that its spectrum is dominated by strong fluorescence lines of Fe as well as continuum emission lines. For physical and geometrical insight into the nature of the reprocessing material, we utilized the high spectroscopic resolving power of the X-ray microcalorimeter (the soft X-ray spectrometer: SXS) and the wide-band sensitivity by the soft and hard X-ray imagers (SXI and HXI) aboard Hitomi. Even though the photon counts are limited due to unintended off-axis pointing, the SXS spectrum resolves Fe Kα1 and Kα2 lines and puts strong constraints on the line centroid and line width. The line width corresponds to a velocity of 160+-37000 km s-1. This represents the most accurate, and smallest, width measurement of this line made so far from the any X-ray binary, much less than the Doppler broadening and Doppler shift expected from speeds that are characteristic of similar systems. Combined with the K-shell edge energy measured by the SXI and HXI spectra, the ionization state of Fe is estimated to be in the range of Fe I-IV. Considering the estimated ionization parameter and the distance between the X-ray source and the absorber, the density and thickness of the materials are estimated. The extraordinarily strong absorption and the absence of a Compton shoulder component have been confirmed. These characteristics suggest reprocessing materials that are distributed in a narrow solid angle or scattering, primarily by warm free electrons or neutral hydrogen. This measurement was achieved using the SXS detection of 19 photons. It provides strong motivation for follow-up observations of this and other X-ray binaries using the X-ray Astrophysics Recovery Mission and other comparable future instruments.","bibtype":"article","author":"Alle, Steven W. and 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 O. 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, Łukasz and Sugawara, Yasuharu and Sugita, Satoshi and Szymkowiak, Andrew and Tajima, Hiroyasu and Takahashi, Hiromitsu and Takahashi, Tadayuki and Takeda, Shiníchiro 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 Suru, Takeshi Got and Uchida, Hiroyuki and Uchiyama, Hideki and Uchiyama, Yasunobu and Ueda, Shutaro and Ueda, Yoshihiro and Uno, Shiníchiro 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 Nakaniwa, Nozomi","journal":"Publications of the Astronomical Society of Japan","number":"2","bibtex":"@article{\n title = {Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi},\n type = {article},\n year = {2018},\n identifiers = {[object Object]},\n keywords = {Binaries: general,Stars: individual (IGR J16318-4848),X-rays: binaries},\n volume = {70},\n websites = {https://academic.oup.com/pasj/article/doi/10.1093/pasj/psx154/4969728},\n month = {3},\n publisher = {Oxford University Press},\n day = {1},\n id = {be53b7b5-8927-3fd6-b8ef-d4b9a66f6a15},\n created = {2018-06-23T07:27:33.792Z},\n accessed = {2018-06-23},\n file_attached = {true},\n profile_id = {ec4888e4-cd9f-3ee0-90a1-39a024d1537d},\n last_modified = {2022-07-15T21:49:30.000Z},\n read = {true},\n starred = {false},\n authored = {true},\n confirmed = {true},\n hidden = {false},\n citation_key = {hitomi18i},\n folder_uuids = {9989056f-58f0-4daf-a99f-4779f0cdd416,5a859072-32ae-4559-8859-863b99a8e32c},\n private_publication = {false},\n abstract = {We report on a Hitomi observation of IGRJ16318-4848, a high-mass X-ray binary system with an extremely strong absorption of NH ∼ 1024cm 2. Previous X-ray studies revealed that its spectrum is dominated by strong fluorescence lines of Fe as well as continuum emission lines. For physical and geometrical insight into the nature of the reprocessing material, we utilized the high spectroscopic resolving power of the X-ray microcalorimeter (the soft X-ray spectrometer: SXS) and the wide-band sensitivity by the soft and hard X-ray imagers (SXI and HXI) aboard Hitomi. Even though the photon counts are limited due to unintended off-axis pointing, the SXS spectrum resolves Fe Kα1 and Kα2 lines and puts strong constraints on the line centroid and line width. The line width corresponds to a velocity of 160+-37000 km s-1. This represents the most accurate, and smallest, width measurement of this line made so far from the any X-ray binary, much less than the Doppler broadening and Doppler shift expected from speeds that are characteristic of similar systems. Combined with the K-shell edge energy measured by the SXI and HXI spectra, the ionization state of Fe is estimated to be in the range of Fe I-IV. Considering the estimated ionization parameter and the distance between the X-ray source and the absorber, the density and thickness of the materials are estimated. The extraordinarily strong absorption and the absence of a Compton shoulder component have been confirmed. These characteristics suggest reprocessing materials that are distributed in a narrow solid angle or scattering, primarily by warm free electrons or neutral hydrogen. This measurement was achieved using the SXS detection of 19 photons. It provides strong motivation for follow-up observations of this and other X-ray binaries using the X-ray Astrophysics Recovery Mission and other comparable future instruments.},\n bibtype = {article},\n author = {Alle, Steven W. and 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 O. 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, Łukasz and Sugawara, Yasuharu and Sugita, Satoshi and Szymkowiak, Andrew and Tajima, Hiroyasu and Takahashi, Hiromitsu and Takahashi, Tadayuki and Takeda, Shiníchiro 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 Suru, Takeshi Got and Uchida, Hiroyuki and Uchiyama, Hideki and Uchiyama, Yasunobu and Ueda, Shutaro and Ueda, Yoshihiro and Uno, Shiníchiro 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 Nakaniwa, Nozomi},\n journal = {Publications of the Astronomical Society of Japan},\n number = {2}\n}","author_short":["Alle, S., W.","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., 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, Ł.","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.","Suru, 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.","Nakaniwa, N."],"urls":{"Website":"https://academic.oup.com/pasj/article/doi/10.1093/pasj/psx154/4969728"},"biburl":"https://bibbase.org/service/mendeley/ec4888e4-cd9f-3ee0-90a1-39a024d1537d","bibbaseid":"alle-aharonian-akamatsu-akimoto-allen-angelini-audard-awaki-etal-glimpseofthehighlyobscuredhmxbigrj163184848withhitomi-2018","role":"author","keyword":["Binaries: general","Stars: individual (IGR J16318-4848)","X-rays: binaries"],"metadata":{"authorlinks":{}},"html":""},"bibtype":"article","biburl":"https://bibbase.org/service/mendeley/ec4888e4-cd9f-3ee0-90a1-39a024d1537d","dataSources":["RmgzPftd92tGag9se"],"keywords":["binaries: general","stars: individual (igr 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of the highly obscured HMXB IGR J16318-4848 with Hitomi","year":2018}