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  • 1. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Canning, Rebecca E. A.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashi, Tasuku
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Shota
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier
    Loewenstein, Michael
    Long, Knox S.
    Lumr, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Norukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemitsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shin'ichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Keigo
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shin'ichiro
    Urry, C. Megan
    Ursino, Eugenio
    Wang, Qian H. S.
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Atmospheric gas dynamics in the Perseus cluster observed with Hitomi2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 9Article in journal (Refereed)
    Abstract [en]

    Extending the earlier measurements reported in Hitomi collaboration (2016, Nature, 535, 117), we examine the atmospheric gas motions within the central 100 kpc of the Perseus cluster using observations obtained with the Hitomi satellite. After correcting for the point spread function of the telescope and using optically thin emission lines, we find that the line-of-sight velocity dispersion of the hot gas is remarkably low and mostly uniform. The velocity dispersion reaches a maxima of approximately 200 km s(-1) toward the central active galactic nucleus (AGN) and toward the AGN inflated northwestern ghost bubble. Elsewhere within the observed region, the velocity dispersion appears constant around 100 km s(-1). We also detect a velocity gradient with a 100 km s(-1) amplitude across the cluster core, consistent with large-scale sloshing of the core gas. If the observed gas motions are isotropic, the kinetic pressure support is less than 10% of the thermal pressure support in the cluster core. The well-resolved, optically thin emission lines have Gaussian shapes, indicating that the turbulent driving scale is likely below 100 kpc, which is consistent with the size of the AGN jet inflated bubbles. We also report the first measurement of the ion temperature in the intracluster medium, which we find to be consistent with the electron temperature. In addition, we present a new measurement of the redshift of the brightest cluster galaxy NGC 1275.

  • 2. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furukawa, Maki
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Kato, Yuichi
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Norukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemitsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shinichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shinichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Temperature structure in the Perseus cluster core observed with Hitomi2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 11Article in journal (Refereed)
    Abstract [en]

    The present paper explains the temperature structure of X-ray emitting plasma in the core of the Perseus cluster based on 1.8-20.0 keV data obtained with the Soft X-ray Spectrometer (SXS) on board the Hitomi Observatory. A series of four observations was carried out, with a total effective exposure time of 338 ks that covered a central region of similar to 7' in diameter. SXS was operated with an energy resolution of similar to 5 eV (full width at half maximum) at 5.9 keV. Not only fine structures of K-shell lines in He-like ions, but also transitions from higher principal quantum numbers were clearly resolved from Si through Fe. That enabled us to perform temperature diagnostics using the line ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of the excitation temperature and ionization temperature in the Perseus cluster. The observed spectrum is roughly reproduced by a single-temperature thermal plasma model in collisional ionization equilibrium, but detailed line-ratio diagnostics reveal slight deviations from this approximation. In particular, the data exhibit an apparent trend of increasing ionization temperature with the atomic mass, as well as small differences between the ionization and excitation temperatures for Fe, the only element for which both temperatures could be measured. The best-fit two-temperature models suggest a combination of 3 and 5 keV gas, which is consistent with the idea that the observed small deviations from a single-temperature approximation are due to the effects of projecting the known radial temperature gradient in the cluster core along the line of sight. A comparison with the Chandra/ACIS and the XMM-Newton/RGS results, on the other hand, suggests that additional lower-temperature components are present in the intracluster medium (ICM), but not detectable with Hitomi/SXS giving its 1.8-20 keV energy band.

  • 3. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furukawa, Maki
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier O.
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Norukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ogorzalek, Anna
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemitsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shinichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shinichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 10Article in journal (Refereed)
    Abstract [en]

    Thanks to its high spectral resolution (similar to 5 eV at 6 keV), the Soft X-ray Spectrometer (SXS) on board Hitomi enables us to measure the detailed structure of spatially resolved emission lines from highly ionized ions in galaxy clusters for the first time. In this series of papers, using the SXS we have measured the velocities of gas motions, metallicities and the multi-temperature structure of the gas in the core of the Perseus Cluster. Here, we show that when inferring physical properties from line emissivities in systems like Perseus, the resonant scattering effect should be taken into account. In the Hitomi waveband, resonant scattering mostly affects the Fe XXV He alpha line (w)-the strongest line in the spectrum. The flux measured by Hitomi in this line is suppressed by a factor of similar to 1.3 in the inner similar to 30 kpc, compared to predictions for an optically thin plasma; the suppression decreases with the distance from the center. The w line also appears slightly broader than other lines from the same ion. The observed distortions of the w line flux, shape, and distance dependence are all consistent with the expected effect of the resonant scattering in the Perseus core. By measuring the ratio of fluxes in optically thick (w) and thin (Fe XXV forbidden, He beta, Ly alpha) lines, and comparing these ratios with predictions from Monte Carlo radiative transfer simulations, the velocities of gas motions have been obtained. The results are consistent with the direct measurements of gas velocities from line broadening described elsewhere in this series, although the systematic and statistical uncertainties remain significant. Further improvements in the predictions of line emissivities in plasma models, and deeper observations with future X-ray missions offering similar or better capabilities to the Hitomi SXS, will enable resonant scattering measurements to provide powerful constraints on the amplitude and anisotropy of cluster gas motions.

  • 4. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguch, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Nobukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sato, Toshiki
    Sawada, Makoto
    Schartel, Norbert
    Serlemtsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shin'ichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shin'ichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Tominaga, Nozomu
    Moriya, Takashi J.
    Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 14Article in journal (Refereed)
    Abstract [en]

    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.

  • 5. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hell, Natalie
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier O.
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Norukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemitsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shin'ichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shin'ichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Raassen, A. J. J.
    Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 12Article in journal (Refereed)
    Abstract [en]

    The Hitomi Soft X-ray Spectrometer spectrum of the Perseus cluster, with similar to 5 eV resolution in the 2-9 keV band, offers an unprecedented benchmark of the atomic modeling and database for hot collisional plasmas. It reveals both successes and challenges of the current atomic data and models. The latest versions of AtomDB/APEC (3.0.8), SPEX (3.03.00), and CHIANTI (8.0) all provide reasonable fits to the broad-band spectrum, and are in close agreement on best-fit temperature, emission measure, and abundances of a few elements such as Ni. For the Fe abundance, the APEC and SPEX measurements differ by 16%, which is 17 times higher than the statistical uncertainty. This is mostly attributed to the differences in adopted collisional excitation and dielectronic recombination rates of the strongest emission lines. We further investigate and compare the sensitivity of the derived physical parameters to the astrophysical source modeling and instrumental effects. The Hitomi results show that accurate atomic data and models are as important as the astrophysical modeling and instrumental calibration aspects. Substantial updates of atomic databases and targeted laboratory measurements are needed to get the current data and models ready for the data from the next Hitomi-level mission.

  • 6. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Nobukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemtsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shinichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Uno, Shinichiro
    Ueda, Yoshihiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Sato, Toshiki
    Nakaniwa, Nozomu
    Murakami, Hiroaki
    Guest, Benson
    Hitomi X-ray observation of the pulsar wind nebula G21.5-0.92018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 3, article id 38Article in journal (Refereed)
    Abstract [en]

    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 Gamma(1) = 1.74 +/- 0.02 and Gamma(2) = 2.14 +/- 0.01 below and above the break at 7.1 +/- 0.3 keV, which is significantly lower than the NuSTAR result (similar to 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 sigma. 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.

  • 7. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Norukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sato, Toshiki
    Sawada, Makoto
    Schartel, Norbert
    Serlemitsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shin'ichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shin'ichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 16Article in journal (Refereed)
    Abstract [en]

    We present Hitomi observations of N 132 D, a young, X-ray bright, O-rich core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily detects the line complexes of highly ionized S K and Fe K with 16-17 counts in each. The Fe feature is measured for the first time at high spectral resolution. Based on the plausible assumption that the Fe K emission is dominated by He-like ions, we find that the material responsible for this Fe emission is highly redshifted at similar to 800 km s(-1) compared to the local LMC interstellar medium (ISM), with a 90% credible interval of 50-1500 km s(-1) if a weakly informative prior is placed on possible line broadening. This indicates (1) that the Fe emission arises from the supernova ejecta, and (2) that these ejecta are highly asymmetric, since no blueshifted component is found. The S K velocity is consistent with the local LMC ISM, and is likely from swept-up ISM material. These results are consistent with spatial mapping that shows the He-like Fe concentrated in the interior of the remnant and the S tracing the outer shell. The results also show that even with a very small number of counts, direct velocity measurements from Doppler-shifted lines detected in extended objects like supernova remnants are now possible. Thanks to the very low SXS background of similar to 1 event per spectral resolution element per 100 ks, such results are obtainable during short pointed or slew observations with similar instruments. This highlights the power of high-spectral-resolution imaging observations, and demonstrates the new window that has been opened with Hitomi and will be greatly widened with future missions such as the X-ray Astronomy Recovery Mission (XARM) and Athena.

  • 8. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    De Plaa, Jelle
    De Vries, Cor P.
    Den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier O.
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Nobukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Oshimizu, Kenya
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemtsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shinichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shinichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Terasawa, Toshio
    Sekido, Mamoru
    Takefuji, Kazuhiro
    Kawai, Eiji
    Misawa, Hiroaki
    Tsuchiya, Fuminori
    Yamazaki, Ryo
    Kobayashi, Eiji
    Kisaka, Shota
    Aoki, Takahiro
    Hitomi X-ray studies of giant radio pulses from the Crab pulsar2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 15Article in journal (Refereed)
    Abstract [en]

    To search for giant X-ray pulses correlated with the giant radio pulses (GRPs) from the Crab pulsar, we performed a simultaneous observation of the Crab pulsar with the X-ray satellite Hitomi in the 2-300 keV band and the Kashima NICT radio telescope in the 1.4-1.7 GHz band with a net exposure of about 2 ks on 2016 March 25, just before the loss of the Hitomi mission. The timing performance of the Hitomi instruments was confirmed to meet the timing requirement and about 1000 and 100 GRPs were simultaneously observed at the main pulse and inter-pulse phases, respectively, and we found no apparent correlation between the giant radio pulses and the X-ray emission in either the main pulse or inter-pulse phase. All variations are within the 2 sigma fluctuations of the X-ray fluxes at the pulse peaks, and the 3 sigma upper limits of variations of main pulse or inter-pulse GRPs are 22% or 80% of the peak flux in a 0.20 phase width, respectively, in the 2-300 keV band. The values for main pulse or inter-pulse GRPs become 25% or 110%, respectively, when the phase width is restricted to the 0.03 phase. Among the upper limits from the Hitomi satellite, those in the 4.5-10 keV and 70-300 keV bands are obtained for the first time, and those in other bands are consistent with previous reports. Numerically, the upper limits of the main pulse and inter-pulse GRPs in the 0.20 phase width are about (2.4 and 9.3) x 10(-11) erg cm(-2), respectively. No significant variability in pulse profiles implies that the GRPs originated from a local place within the magneto-sphere. Although the number of photon-emitting particles should temporarily increase to account for the brightening of the radio emission, the results do not statistically rule out variations correlated with the GRPs, because the possible X-ray enhancement may appear due to a > 0.02% brightening of the pulse-peak flux under such conditions.

  • 9. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier O.
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Norukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemitsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shin'ichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shin'ichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Kawamuro, Taiki
    Hitomi observation of radio galaxy NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-K alpha line emission from an active galactic nucleus2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 13Article in journal (Refereed)
    Abstract [en]

    The origin of the narrow Fe-K alpha fluorescence line at 6.4 keV from active galactic nuclei has long been under debate; some of the possible sites are the outer accretion disk, the broad line region, a molecular torus, or interstellar/intracluster media. In 2016 February-March, we performed the first X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS) on board the Hitomi satellite of the Fanaroff-Riley type I radio galaxy NGC 1275 at the center of the Perseus cluster of galaxies. With the high-energy resolution of similar to 5 eV at 6 keV achieved by Hitomi/SXS, we detected the Fe-K alpha line with similar to 5.4 sigma significance. The velocity width is constrained to be 500-1600 km s(-1) (FWHM for Gaussian models) at 90% confidence. The SXS also constrains the continuum level from the NGC 1275 nucleus up to similar to 20 keV, giving an equivalent width of similar to 20 eV for the 6.4 keV line. Because the velocity width is narrower than that of the broad H alpha line of similar to 2750 km s(-1), we can exclude a large contribution to the line flux from the accretion disk and the broad line region. Furthermore, we performed pixel map analyses on the Hitomi/SXS data and image analyses on the Chandra archival data, and revealed that the Fe-K alpha line comes from a region within similar to 1.6 kpc of the NGC 1275 core, where an active galactic nucleus emission dominates, rather than that from intracluster media. Therefore, we suggest that the source of the Fe-K alpha line from NGC 1275 is likely a low-covering-fraction molecular torus or a rotating molecular disk which probably extends from a parsec to hundreds of parsecs scale in the active galactic nucleus system.

  • 10. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier O.
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Norukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemitsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shinichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shinichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Nakaniwa, Nozomi
    Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 2, article id 17Article in journal (Refereed)
    Abstract [en]

    We report on a Hitomi observation of IGR J16318-4848, a high-mass X-ray binary system with an extremely strong absorption of N-H similar to 10(24) cm(-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 K alpha(1) and K alpha(2) lines and puts strong constraints on the line centroid and line width. The line width corresponds to a velocity of 160(-70)(+300) 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.

  • 11. Aharonian, Felix
    et al.
    Akamatsu, Hiroki
    Akimoto, Fumie
    Allen, Steven W.
    Angelini, Lorella
    Audard, Marc
    Awaki, Hisamitsu
    Axelsson, Magnus
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Bamba, Aya
    Bautz, Marshall W.
    Blandford, Roger
    Brenneman, Laura W.
    Brown, Gregory V.
    Bulbul, Esra
    Cackett, Edward M.
    Chernyakova, Maria
    Chiao, Meng P.
    Coppi, Paolo S.
    Costantini, Elisa
    de Plaa, Jelle
    de Vries, Cor P.
    den Herder, Jan-Willem
    Done, Chris
    Dotani, Tadayasu
    Ebisawa, Ken
    Eckart, Megan E.
    Enoto, Teruaki
    Ezoe, Yuichiro
    Fabian, Andrew C.
    Ferrigno, Carlo
    Foster, Adam R.
    Fujimoto, Ryuichi
    Fukazawa, Yasushi
    Furuzawa, Akihiro
    Galeazzi, Massimiliano
    Gallo, Luigi C.
    Gandhi, Poshak
    Giustini, Margherita
    Goldwurm, Andrea
    Gu, Liyi
    Guainazzi, Matteo
    Haba, Yoshito
    Hagino, Kouichi
    Hamaguchi, Kenji
    Harrus, Ilana M.
    Hatsukade, Isamu
    Hayashi, Katsuhiro
    Hayashi, Takayuki
    Hayashida, Kiyoshi
    Hiraga, Junko S.
    Hornschemeier, Ann
    Hoshino, Akio
    Hughes, John P.
    Ichinohe, Yuto
    Iizuka, Ryo
    Inoue, Hajime
    Inoue, Yoshiyuki
    Ishida, Manabu
    Ishikawa, Kumi
    Ishisaki, Yoshitaka
    Iwai, Masachika
    Kaastra, Jelle
    Kallman, Tim
    Kamae, Tsuneyoshi
    Kataoka, Jun
    Katsuda, Satoru
    Kawai, Nobuyuki
    Kelley, Richard L.
    Kilbourne, Caroline A.
    Kitaguchi, Takao
    Kitamoto, Shunji
    Kitayama, Tetsu
    Kohmura, Takayoshi
    Kokubun, Motohide
    Koyama, Katsuji
    Koyama, Shu
    Kretschmar, Peter
    Krimm, Hans A.
    Kubota, Aya
    Kunieda, Hideyo
    Laurent, Philippe
    Lee, Shiu-Hang
    Leutenegger, Maurice A.
    Limousin, Olivier
    Loewenstein, Michael
    Long, Knox S.
    Lumb, David
    Madejski, Greg
    Maeda, Yoshitomo
    Maier, Daniel
    Makishima, Kazuo
    Markevitch, Maxim
    Matsumoto, Hironori
    Matsushita, Kyoko
    McCammon, Dan
    McNamara, Brian R.
    Mehdipour, Missagh
    Miller, Eric D.
    Miller, Jon M.
    Mineshige, Shin
    Mitsuda, Kazuhisa
    Mitsuishi, Ikuyuki
    Miyazawa, Takuya
    Mizuno, Tsunefumi
    Mori, Hideyuki
    Mori, Koji
    Mukai, Koji
    Murakami, Hiroshi
    Mushotzky, Richard F.
    Nakagawa, Takao
    Nakajima, Hiroshi
    Nakamori, Takeshi
    Nakashima, Shinya
    Nakazawa, Kazuhiro
    Nobukawa, Kumiko K.
    Nobukawa, Masayoshi
    Noda, Hirofumi
    Odaka, Hirokazu
    Ohashi, Takaya
    Ohno, Masanori
    Okajima, Takashi
    Ota, Naomi
    Ozaki, Masanobu
    Paerels, Frits
    Paltani, Stephane
    Petre, Robert
    Pinto, Ciro
    Porter, Frederick S.
    Pottschmidt, Katja
    Reynolds, Christopher S.
    Safi-Harb, Samar
    Saito, Shinya
    Sakai, Kazuhiro
    Sasaki, Toru
    Sato, Goro
    Sato, Kosuke
    Sato, Rie
    Sawada, Makoto
    Schartel, Norbert
    Serlemtsos, Peter J.
    Seta, Hiromi
    Shidatsu, Megumi
    Simionescu, Aurora
    Smith, Randall K.
    Soong, Yang
    Stawarz, Lukasz
    Sugawara, Yasuharu
    Sugita, Satoshi
    Szymkowiak, Andrew
    Tajima, Hiroyasu
    Takahashi, Hiromitsu
    Takahashi, Tadayuki
    Takeda, Shin'ichiro
    Takei, Yoh
    Tamagawa, Toru
    Tamura, Takayuki
    Tanaka, Takaaki
    Tanaka, Yasuo
    Tanaka, Yasuyuki T.
    Tashiro, Makoto S.
    Tawara, Yuzuru
    Terada, Yukikatsu
    Terashima, Yuichi
    Tombesi, Francesco
    Tomida, Hiroshi
    Tsuboi, Yohko
    Tsujimoto, Masahiro
    Tsunemi, Hiroshi
    Tsuru, Takeshi Go
    Uchida, Hiroyuki
    Uchiyama, Hideki
    Uchiyama, Yasunobu
    Ueda, Shutaro
    Ueda, Yoshihiro
    Uno, Shin'ichiro
    Urry, C. Megan
    Ursino, Eugenio
    Watanabe, Shin
    Werner, Norbert
    Wilkins, Dan R.
    Williams, Brian J.
    Yamada, Shinya
    Yamaguchi, Hiroya
    Yamaoka, Kazutaka
    Yamasaki, Noriko Y.
    Yamauchi, Makoto
    Yamauchi, Shigeo
    Yaqoob, Tahir
    Yatsu, Yoichi
    Yonetoku, Daisuke
    Zhuravleva, Irina
    Zoghbi, Abderahmen
    Uchida, Yuusuke
    Detection of polarized gamma-ray emission from the Crab nebula with the Hitomi Soft Gamma-ray Detector2018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 6, article id psy113Article in journal (Refereed)
    Abstract [en]

    We present the results from the Hitomi Soft Gamma-ray Detector (SGD) observation of the Crab nebula. The main part of SGD is a Compton camera, which in addition to being a spectrometer, is capable of measuring polarization of gamma-ray photons. The Crab nebula is one of the brightest X-ray / gamma-ray sources on the sky, and, the only source from which polarized X-ray photons have been detected. SGD observed the Crab nebula during the initial test observation phase of Hitomi. We performed the data analysis of the SGD observation, the SGD background estimation and the SGD Monte Carlo simulations, and, successfully detected polarized gamma-ray emission from the Crab nebula with only about 5 ks exposure time. The obtained polarization fraction of the phase-integrated Crab emission (sum of pulsar and nebula emissions) is (22.1% +/- 10.6%), and, the polarization angle is 110.degrees 7 + 13.degrees 2 /-13.degrees 0 in the energy range of 60-160 keV (The errors correspond to the 1 sigma deviation). The confidence level of the polarization detection was 99.3%. The polarization angle measured by SGD is about one sigma deviation with the projected spin axis of the pulsar, 124.degrees 0 +/- 0.degrees 1.

  • 12. Kato, Yuta
    et al.
    Matsuda, Yuichi
    Iono, Daisuke
    Hatsukade, Bunyo
    Umehata, Hideki
    Kohno, Kotaro
    Alexander, David M.
    Ao, Yiping
    Chapman, Scott C.
    Hayes, Matthew
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Kubo, Mariko
    Lehmer, Bret D.
    Malkan, Matthew A.
    Michiyama, Tomonari
    Nagao, Tohru
    Saito, Tomoki
    Tanaka, Ichi
    Taniguchi, Yoshiaki
    A high dust emissivity index beta for a CO-faint galaxy in a filamentary Ly alpha nebula at z=3.12018In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 70, no 5, article id L6Article in journal (Refereed)
    Abstract [en]

    We present CO J = 4-3 line and 3 mm dust continuum observations of a 100 kpc-scale filamentary Ly alpha nebula (SSA22 LAB18) at z = 3.1 using the Atacama Large Millimeter/submillimeter Array (ALMA). We detected the CO J = 4-3 line at a systemic z(CO) = 3.093 +/- 0.001 at 11 sigma from one of the ALMA continuum sources associated with the Ly alpha filament. We estimated the CO J = 4-3 luminosity of L'(CO(4-3)) = (2.3 +/- 0.2) x 10(9) Kkms(-1) pc(2) for this CO source, which is one order of magnitude smaller than those of typical z > 1 dusty star-forming galaxies (DSFGs) of similar far-infrared luminosity L-IR similar to 10(12) L-circle dot. We derived a molecular gas mass of M-gas = (4.4(-0.6)(+0.9)) x 10(9) M-circle dot and a star-formation rate of SFR = 270 +/- 160M(circle dot) yr(-1). We also estimated a gas depletion time of tau(dep) = 17 +/- 10 Myr, which is shorter than those of typical DSFGs. It is suggested that this source is in the transition phase from DSFG to a gas-poor, early-type galaxy. From ALMA to Herschel multi-band dust continuum observations, we measured a dust emissivity index beta = 2.3 +/- 0.2, which is similar to those of local gas-poor, early-type galaxies. From recent laboratory experiments, the specific chemical compositions needed to reproduce such a high beta for interstellar dust at the submillimeter wavelengths. ALMA CO and multi-band dust continuum observations can constrain the evolutionary stage of high-redshift galaxies through tau(dep) and beta, and thus we can investigate the chemical composition of dust even in the early Universe.

  • 13. Momose, Munetake
    et al.
    Morita, Ayaka
    Fukagawa, Misato
    Muto, Takayuki
    Takeuchi, Taku
    Hashimoto, Jun
    Honda, Mitsuhiko
    Kudo, Tomoyuki
    Okamoto, Yoshiko K.
    Kanagawa, Kazuhiro D.
    Tanaka, Hidekazu
    Grady, Carol A.
    Sitko, Michael L.
    Akiyama, Eiji
    Currie, Thayne
    Follette, Katherine B.
    Mayama, Satoshi
    Kusakabe, Nobuhiko
    Abe, Lyu
    Brandner, Wolfgang
    Brandt, Timothy D.
    Carson, Joseph C.
    Egner, Sebastian
    Feldt, Markus
    Goto, Miwa
    Guyon, Olivier
    Hayano, Yutaka
    Hayashi, Masahiko
    Hayashi, Saeko S.
    Henning, Thomas
    Hodapp, Klaus W.
    Ishii, Miki
    Iye, Masanori
    Janson, Markus
    Stockholm University, Faculty of Science, Department of Astronomy.
    Kandori, Ryo
    Knapp, Gillian R.
    Kuzuhara, Masayuki
    Kwon, Jungmi
    Matsuo, Taro
    McElwain, Michael W.
    Miyama, Shoken
    Morino, Jun-Ichi
    Moro-Martin, Amaya
    Nishimura, Tetsuo
    Pyo, Tae-Soo
    Serabyn, Eugene
    Suenaga, Takuya
    Suto, Hiroshi
    Suzuki, Ryuji
    Takahashi, Yasuhiro H.
    Takami, Michihiro
    Takato, Naruhisa
    Terada, Hiroshi
    Thalmann, Christian
    Tomono, Daigo
    Turner, Edwin L.
    Watanabe, Makoto
    Wisniewski, John
    Yamada, Toru
    Takami, Hideki
    Usuda, Tomonori
    Tamura, Motohide
    Detailed structure of the outer disk around HD169142 with polarized light in H-band2015In: Nippon Tenmon Gakkai obun kenkyu hokoku, ISSN 0004-6264, Vol. 67, no 5, article id 83Article in journal (Refereed)
    Abstract [en]

    Coronagraphic imagery of the circumstellar disk around HD 169142 in H-band polarized intensity (PI) with Subaru/HiCIAO is presented. The emission scattered by dust particles at the disk surface in 0.2 <= r <= 1.2, or 29 <= r <= 174 AU, is successfully detected. The azimuthally-averaged radial profile of the PI shows a double power-law distribution, in which the PIs in r=29-52 AU and r=81.2-145 AU respectively show r(-3)-dependence. These two power-law regions are connected smoothly with a transition zone (TZ), exhibiting an apparent gap in r=40-70 AU. The PI in the inner power-law region shows a deep minimum whose location seems to coincide with the point source at lambda = 7 mm. This can be regarded as another sign of a protoplanet in TZ. The observed radial profile of the PI is reproduced by a minimally flaring disk with an irregular surface density distribution or with an irregular temperature distribution or with the combination of both. The depletion factor of surface density in the inner power-law region (r<50 AU) is derived to be >= 0.16 from a simple model calculation. The obtained PI image also shows small scale asymmetries in the outer power-law region. Possible origins for these asymmetries include corrugation of the scattering surface in the outer region, and shadowing effect by a puffed up structure in the inner power-law region.

  • 14. Morokuma, Tomoki
    et al.
    Tanaka, Masaomi
    Tanaka, Yasuyuki T.
    Itoh, Ryosuke
    Tominaga, Nozomu
    Gandhi, Poshak
    Pian, Elena
    Mazzali, Paolo
    Ohta, Kouji
    Matsumoto, Emiko
    Shibata, Takumi
    Akimoto, Hinako
    Akitaya, Hiroshi
    Ali, Gamal B.
    Aoki, Tsutomu
    Doi, Mamoru
    Ebisuda, Nana
    Essam, Ahmed
    Fujisawa, Kenta
    Fukushima, Hideo
    Goda, Shuhei
    Gouda, Yuya
    Hanayama, Hidekazu
    Hashiba, Yasuhito
    Hashimoto, Osamu
    Hayashida, Kenzo
    Hiratsuka, Yuichiro
    Honda, Satoshi
    Imai, Masataka
    Inoue, Kanichiro
    Ishibashi, Michiko
    Iwata, Ikuru
    Izumiura, Hideyuki
    Kanda, Yuka
    Kawabata, Miho
    Kawaguchi, Kenji
    Kawai, Nobuyuki
    Kokubo, Mitsuru
    Kuroda, Daisuke
    Maehara, Hiroyuki
    Mito, Hiroyuki
    Mitsuda, Kazuma
    Miyagawa, Ryota
    Miyaji, Takeshi
    Miyamoto, Yusuke
    Morihana, Kumiko
    Moritani, Yuki
    Morokuma-Matsui, Kana
    Murakami, Kotone
    Murata, Katsuhiro L.
    Nagayama, Takahiro
    Nakamura, Kazuki
    Nakaoka, Tatsuya
    Niinuma, Kotaro
    Nishimori, Takafumi
    Nogami, Daisaku
    Oasa, Yumiko
    Oda, Tatsunori
    Ohshima, Tomohito
    Saito, Yoshihiko
    Sakata, Shuichiro
    Sako, Shigeyuki
    Sarugaku, Yuki
    Sawada-Satoh, Satoko
    Seino, Genta
    Sorai, Kazuo
    Soyano, Takao
    Taddia, Francesco
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Takahashi, Jun
    Takagi, Yuhei
    Takaki, Katsutoshi
    Takata, Koji
    Tarusawa, Ken'ichi
    Uemura, Makoto
    Ui, Takahiro
    Urago, Riku
    Ushioda, Kazutoshi
    Watanabe, Jun-ichi
    Watanabe, Makoto
    Yamashita, Satoshi
    Yanagisawa, Kenshi
    Yonekura, Yoshinori
    Yoshida, Michitoshi
    OISTER optical and near-infrared monitoring observations of peculiar radio-loud active galactic nucleus SDSSJ110006.07+442144.32017In: Nippon Tenmon Gakkai obun kenkyu hokoku, ISSN 0004-6264, Vol. 69, no 5, article id 82Article in journal (Refereed)
    Abstract [en]

    We present monitoring campaign observations at optical and near-infrared (NIR) wavelengths for a radio-loud active galactic nucleus (AGN) at z = 0.840, SDSSJ110006.07+442144.3 (hereafter, J1100+4421), which was identified during a flare phase in late 2014 February. The campaigns consist of three intensive observing runs from the discovery to 2015 March, mostly within the scheme of the OISTER collaboration. Optical-NIR light curves and simultaneous spectral energy distributions (SEDs) are obtained. Our measurements show the strongest brightening in 2015 March. We found that the optical-NIR SEDs of J1100+4421 show an almost steady shape despite the large and rapid intranight variability. This constant SED shape is confirmed to extend to similar to 5 mu m in the observed frame using the archival WISE data. Given the lack of absorption lines and the steep power-law spectrum of alpha(upsilon) similar to -1.4, where f(v) proportional to v(alpha upsilon), synchrotron radiation by a relativistic jet with no or small contributions from the host galaxy and the accretion disk seemsmost plausible as an optical-NIR emission mechanism. The steep optical-NIR spectral shape and the large amplitude of variability are consistent with this object being a low.peak jet-dominated AGN. In addition, sub-arcsecond resolution optical imaging data taken with Subaru Hyper Suprime-Cam does not show a clear extended component and the spatial scales are significantly smaller than the large extensions detected at radio wavelengths. The optical spectrum of a possible faint companion galaxy does not show any emission lines at the same redshift, and hence a merging hypothesis for this AGN-related activity is not supported by our observations.

  • 15. Morokuma, Tomoki
    et al.
    Tokita, Kouichi
    Lidman, Christopher
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Doi, Mamoru
    Yasuda, Naoki
    Aldering, Greg
    Amanullah, Rahman
    Stockholm University, Faculty of Science, Department of Physics.
    Barbary, Kyle
    Dawson, Kyle
    Fadeyev, Vitaliy
    Fakhouri, Hannah K.
    Goldhaber, Gerson
    Goobar, Ariel
    Stockholm University, Faculty of Science, Department of Physics.
    Hattori, Takashi
    Hayano, Junji
    Hook, Isobel M.
    Howell, D. Andrew
    Furusawa, Hisanori
    Ihara, Yutaka
    Kashikawa, Nobunari
    Knop, Rob A.
    Konishi, Kohki
    Meyers, Joshua
    Oda, Takeshi
    Pain, Reynald
    Perlmutter, Saul
    Rubin, David
    Spadafora, Anthony L.
    Suzuki, Nao
    Takanashi, Naohiro
    Totani, Tomonori
    Utsunomiya, Hiroyuki
    Wang, Lifan
    Subaru FOCAS Spectroscopic Observations of High-Redshift Supernovae2010In: Nippon Tenmon Gakkai obun kenkyu hokoku, ISSN 0004-6264, Vol. 62, no 1, p. 19-37Article in journal (Refereed)
    Abstract [en]

    We present spectra of high-redshift supernovae (SNe) that were taken with the Subaru low-resolution optical spectrograph, FOCAS. These SNe were found in SN surveys with Suprime-Cam on Subaru, the CFH12k camera on the Canada-France-Hawaii Telescope, and the Advanced Camera for Surveys on the Hubble Space Telescope. These SN surveys specifically targeted z > 1 Type la supernovae (SNe Ia). From the spectra of 39 candidates, we obtained redshifts for 32 candidates and spectroscopically identified 7 active candidates as probable SNe Ia, including one at z = 1.35, which is the most distant SN la to be spectroscopically confirmed with a ground-based telescope. An additional 4 candidates were identified as likely SNe la from the spectrophotometric properties of their host galaxies. Seven candidates are not SNe la, either being SNe of another type or active galactic nuclei. When SNe la were observed within one week of the maximum light, we found that we could spectroscopically identify most of them up to z = 1.1. Beyond this redshift, very few candidates were spectroscopically identified as SNe Ia. The current generation of super red-sensitive, fringe-free CCDs will push this redshift limit higher.

  • 16. Morokuma, Tomoki
    et al.
    Tominaga, Nozomu
    Tanaka, Masaomi
    Mori, Kensho
    Matsumoto, Emiko
    Kikuchi, Yuki
    Shibata, Takumi
    Sako, Shigeyuki
    Aoki, Tsutomu
    Doi, Mamoru
    Kobayashi, Naoto
    Maehara, Hiroyuki
    Matsunaga, Noriyuki
    Mito, Hiroyuki
    Miyata, Takashi
    Nakada, Yoshikazu
    Soyano, Takao
    Tarusawa, Ken'ichi
    Miyazaki, Satoshi
    Nakata, Fumiaki
    Okada, Norio
    Sarugaku, Yuki
    Richmond, Michael W.
    Akitaya, Hiroshi
    Aldering, Greg
    Arimatsu, Ko
    Contreras, Carlos
    Hortiuchi, Takashi
    Hsiao, Eric Y.
    Itoh, Ryosuke
    Iwata, Ikuru
    Kawabata, Koji S.
    Kawai, Nobuyuki
    Kitagawa, Yutaro
    Kokubo, Mitsuru
    Kuroda, Daisuke
    Mazzali, Paolo
    Misawa, Toru
    Moritani, Yuki
    Morrell, Nidia
    Okamoto, Rina
    Pavlyuk, Nikolay
    Phillips, Mark M.
    Pian, Elena
    Sahu, Devendra
    Saito, Yoshihiko
    Sano, Kei
    Stritzinger, Maximilian D.
    Tachibana, Yutaro
    Taddia, Francesco
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Takaki, Katsutoshi
    Tateuchi, Ken
    Tomita, Akihiko
    Tsvetkov, Dmitry
    Ui, Takahiro
    Ukita, Nobuharu
    Urata, Yuji
    Walker, Emma S.
    Yoshii, Taketoshi
    Kiso Supernova Survey (KISS): Survey strategy2014In: Nippon Tenmon Gakkai obun kenkyu hokoku, ISSN 0004-6264, Vol. 66, no 6, article id 114Article in journal (Refereed)
    Abstract [en]

    lThe Kiso Supernova Survey (KISS) is a high-cadence optical wide-field supernova (SN) survey. The primary goal of the survey is to catch the very early light of a SN, during the shock breakout phase. Detection of SN shock breakouts combined with multi-band photometry obtained with other facilities would provide detailed physical information on the progenitor stars of SNe. The survey is performed using a 2 degrees.2 x 2 degrees.2 field-of-view instrument on the 1.05-m Kiso Schmidt telescope, the Kiso Wide Field Camera (KWFC). We take a 3-min exposure in g-band once every hour in our survey, reaching magnitude g similar to 20-21. About 100 nights of telescope time per year have been spent on the survey since 2012 April. The number of the shock breakout detections is estimated to be of the order of 1 during our three-year project. This paper summarizes the KISS project including the KWFC observing setup, the survey strategy, the data reduction system, and CBET-reported SNe discovered so far by KISS.

  • 17. Ohta, Yurina
    et al.
    Fukagawa, Misato
    Sitko, Michael L.
    Muto, Takayuki
    Kraus, Stefan
    Grady, Carol A.
    Wisniewski, John P.
    Swearingen, Jeremy R.
    Shibai, Hiroshi
    Sumi, Takahiro
    Hashimoto, Jun
    Kudo, Tomoyuki
    Kusakabe, Nobuhiko
    Momose, Munetake
    Okamoto, Yoshiko
    Kotani, Takayuki
    Takami, Michihiro
    Currie, Thayne
    Thalmann, Christian
    Janson, Markus
    Stockholm University, Faculty of Science, Department of Astronomy.
    Akiyama, Eiji
    Follette, Katherine B.
    Mayama, Satoshi
    Abe, Lyu
    Brandner, Wolfgang
    Brandt, Timothy D.
    Carson, Joseph C.
    Egner, Sebastian E.
    Feldt, Markus
    Goto, Miwa
    Guyon, Olivier
    Hayano, Yutaka
    Hayashi, Masahiko
    Hayashi, Saeko S.
    Henning, Thomas
    Hodapp, Klaus W.
    Ishii, Miki
    Iye, Masanori
    Kandori, Ryo
    Knapp, Gillian R.
    Kuzuhara, Masayuki
    Kwon, Jungmi
    Matsuo, Taro
    McElwain, Michael W.
    Miyama, Shoken
    Morino, Jun-Ichi
    Moro-Martin, Amaya
    Nishimura, Tetsuo
    Pyo, Tae-Soo
    Serabyn, Eugene
    Suenaga, Takuya
    Suto, Hiroshi
    Suzuki, Ryuji
    Takahashi, Yasuhiro H.
    Takami, Hideki
    Takato, Naruhisa
    Terada, Hiroshi
    Tomono, Daigo
    Turner, Edwin L.
    Usuda, Tomonori
    Watanabe, Makoto
    Yamada, Toru
    Tamura, Motohide
    Extreme asymmetry in the polarized disk of V1247 Orionis2016In: Nippon Tenmon Gakkai obun kenkyu hokoku, ISSN 0004-6264, Vol. 68, no 4, article id 53Article in journal (Refereed)
    Abstract [en]

    We present the first near-infrared scattered-light detection of the transitional disk around V1247 Ori, which was obtained using high-resolution polarimetric differential imaging observations with Subaru/HiCIAO. Our imaging in the H band reveals the disk morphology at separations of similar to 0.'' 14-0.'' 86 (54-330 au) from the central star. The polarized intensity image shows a remarkable arc-like structure toward the southeast of the star, whereas the fainter northwest region does not exhibit any notable features. The shape of the arm is consistent with an arc of 0.'' 28 +/- 0.'' 09 in radius (108 au from the star), although the possibility of a spiral arm with a small pitch angle cannot be excluded. V1247 Ori features an exceptionally large azimuthal contrast in scattered, polarized light; the radial peak of the southeastern arc is about three times brighter than the northwestern disk measured at the same distance from the star. Combined with the previous indication of an inhomogeneous density distribution in the gap at less than or similar to 46 au, the notable asymmetry in the outer disk suggests the presence of unseen companions and/or planet-forming processes ongoing in the arc.

1 - 17 of 17
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