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  2. 辻本 匡弘

辻本 匡弘

ツジモト マサヒロ  (Masahiro Tsujimoto)

基本情報

所属
国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 准教授
学位
博士（理学）(2003年3月 京都大学)
修士（理学）(2000年3月 京都大学)
連絡先
tsujimoto.masahirojaxa.jp
研究者番号
10528178
ORCID ID
 https://orcid.org/0000-0002-9184-5556
J-GLOBAL ID
201801010256574610
Researcher ID
ABC-6667-2020
researchmap会員ID
B000296937
外部リンク

研究キーワード

 6

研究分野

 2

経歴

 5

学歴

 3

委員歴

 1

論文

 261
  • Yuto Mochizuki, Masahiro Tsujimoto, Maurice A Leutenegger, Liyi Gu, Ralf Ballhausen, Ehud Behar, Paul A Draghis, Natalie Hell, Pragati Pradhan
    Publications of the Astronomical Society of Japan 2025年9月30日  
  • Miki Kurihara, Masahiro Tsujimoto, Marc Audard, Ehud Behar, Liyi Gu, Kenji Hamaguchi, Natalie Hell, Caroline A Kilbourne, Yoshitomo Maeda, Frederick S Porter, Haruka Sugai, Yohko Tsuboi
    Publications of the Astronomical Society of Japan 2025年9月30日  
  • Masahiro Tsujimoto, Teruaki Enoto, María Díaz Trigo, Natalie Hell, Priyanka Chakraborty, Maurice A Leutenegger, Michael Loewenstein, Pragati Pradhan, Megumi Shidatsu, Hiromitsu Takahashi, Tahir Yaqoob
    Publications of the Astronomical Society of Japan 2025年9月30日  
  • Kurihara, Miki, Tsujimoto, Masahiro, Audard, Marc, Behar, Ehud, Gu, Liyi, Hamaguchi, Kenji, Hell, Natalie, Kilbourne, Caroline A., Maeda, Yoshitomo, Porter, Frederick S., Sugai, Haruka, Tsuboi, Yohko
    2025年4月  
    The RS CVn type binary star GT Mus was observed during its quiescence using the Resolve X-ray microcalorimeter spectrometer onboard XRISM. The main and satellite lines of the Fe XXIV--XXVI K-shell transitions were resolved for the first time from stellar sources. We conducted line ratio analysis to investigate any deviations from collisional onization equilibrium (CIE) and Maxwell electron energy distribution with a single-temperature. By using five combinations of direct excitation lines and dielectronic recombination satellite lines in three line complexes (Fe He$α$, Ly$α$, and He$β$), we found that the plasma is well characterized by two-temperature thermal plasmas with temperatures of 1.7 and 4.3 keV, which is consistent with a thermal broadening of Fe XXV and the broadband fitting results in the 1.7--10 keV band. Other forms of deviation from a single-temperature plasma, such as different ionization and electron temperatures or the $κ$ distribution for the electron energy distributions, are not favored, which is reasonable for stellar coronae at quiescence. This study demonstrates the utility of the Fe K-shell line ratio diagnostics to probe plasma conditions using X-ray microcalorimeters....
  • Tsujimoto, Masahiro, Enoto, Teruaki, Díaz Trigo, María, Hell, Natalie, Chakraborty, Priyanka, Leutenegger, Maurice A., Loewenstein, Michael, Pradhan, Pragati, Shidatsu, Megumi, Takahashi, Hiromitsu, Yaqoob, Tahir
    2025年3月  
    High-resolution X-ray spectroscopy is a key to understanding the mass inflow and outflow of compact objects. Spectral lines carry information about the ionization, density, and velocity structures through their intensity ratios and profiles. They are formed in non-local thermodynamic equilibrium conditions under the intense radiation field from the compact objects, thus radiative transfer (RT) calculation is a requisite for proper interpretations. We present such a study for a low-mass X-ray binary, Circinus X-1, from which the P Cygni profile was discovered using the X-ray grating spectrometer onboard Chandra. We observed the source using the X-ray microcalorimeter onboard XRISM at an orbital phase of 0.93-0.97 and revealed many spectral features unidentified before; the higher series transitions (n to 1; n > 2) of highly-ionized (H- and He-like) S, Ca, Ar, and Fe in emission and absorption, the Fe K{\alpha} and K\b{eta} inner-shell excitation absorption of mildly-ionized (O- to Li-like) Fe, and resolved fine-structure level transitions in the Fe Ly{\alpha} and He{\alpha} complexes. They blend with each other at different velocity shifts on top of apparently variable continuum emission that changed its flux by an order of magnitude within a 70 ks telescope time. Despite such complexity in the observed spectra, most of them can be explained by a simple model consisting of the photoionized plasma outflowing at ~300 km s-1 and the variable blocking material in the line of sight of the incident continuum emission from the accretion disk. We demonstrate this with the aid of the RT code cloudy for the line ratio diagnostics and spectral fitting. We further constrain the physical parameters of the outflow and argue that the outflow is launched close to the outer edge of the accretion disk and can be driven radiatively by being assisted by the line force calculated using the RT simulation....
  • Xrism Collaboration, Audard, Marc, Awaki, Hisamitsu, Ballhausen, Ralf, Bamba, Aya, Behar, Ehud, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V., Corrales, Lia, Costantini, Elisa, Cumbee, Renata, Diaz Trigo, Maria, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Eckert, Dominique, Eguchi, Satoshi, Enoto, Teruaki, Ezoe, Yuichiro, Foster, Adam, Fujimoto, Ryuichi, Fujita, Yutaka, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, García, Javier A., Gu, Liyi, Guainazzi, Matteo, Hagino, Kouichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Hornschemeier, Ann, Ichinohe, Yuto, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Timothy, Kara, Erin, Katsuda, Satoru, Kanemaru, Yoshiaki, Kelley, Richard, Kilbourne, Caroline, Kitamoto, Shunji, Kobayashi, Shogo, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Loewenstein, Michael, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Mernier, François, Miller, Eric D., Miller, Jon M., Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakajima, Hiroshi, Nakazawa, Kazuhiro, Ness, Jan-Uwe, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Shoji, Ogorzalek, Anna, Okajima, Takashi, Ota, Naomi, Paltani, Stephane, Petre, Robert, Plucinsky, Paul, Porter, Frederick S., Pottschmidt, Katja, Sato, Kosuke, Sato, Toshiki, Sawada, Makoto, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall, Suzuki, Hiromasa, Szymkowiak, Andrew, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Tashiro, Makoto, Terada, Yukikatsu, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Vink, Jacco, Watanabe, Shin, Williams, Brian J., Yamada, Satoshi, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yoneyama, Tomokage, Yoshida, Tessei, Yukita, Mihoko, Zhuravleva, Irina, Bartalesi, Tommaso, Ettori, Stefano, Kosarzycki, Roman, Lovisari, Lorenzo, Rose, Tom, Sarkar, Arnab, Sun, Ming, Tamhane, Prathamesh
    The Astrophysical Journal 2025年3月  
    We present XRISM Resolve observations of the core of the hot, relaxed galaxy cluster Abell 2029 (A2029). We find that the line-of-sight bulk velocity of the intracluster medium (ICM) within the central 180 kpc is at rest with respect to the brightest cluster galaxy, with a 3σ upper limit of ∣vbulk∣ &lt; 100 km s‑1. We robustly measure the field-integrated ICM velocity dispersion to be σv = 169 ± 10 km s‑1, obtaining similar results for both single-temperature and two-temperature plasma models to account for the cluster cool core. This result, if ascribed to isotropic turbulence, implies a subsonic ICM with Mach number <inline-formula> </inline-formula> and a nonthermal pressure fraction of 2.6 ± 0.3%. The turbulent velocity is similar to what was measured in the core of the Perseus cluster by Hitomi, but here in a more massive cluster with an ICM temperature of 7 keV, the limit on the nonthermal pressure fraction is even more stringent. Our result is consistent with expectations from simulations of relaxed clusters, but it is on the low end of the predicted distribution, indicating that A2029 is an exceptionally relaxed cluster with no significant impacts from either a recent minor merger or active galactic nucleus activity....
  • XRISM Collaboration, Audard, Marc, Awaki, Hisamitsu, Ballhausen, Ralf, Bamba, Aya, Behar, Ehud, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V, Corrales, Lia, Costantini, Elisa, Cumbee, Renata, Diaz-Trigo, Maria, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan, Eckert, Dominique, Enoto, Teruaki, Eguchi, Satoshi, Ezoe, Yuichiro, Foster, Adam, Fujimoto, Ryuichi, Fujita, Yutaka, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, García, Javier A, Gu, Liyi, Guainazzi, Matteo, Hagino, Kouichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Hornschemeier, Ann, Ichinohe, Yuto, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Timothy, Kara, Erin, Katsuda, Satoru, Kanemaru, Yoshiaki, Kelley, Richard, Kilbourne, Caroline, Kitamoto, Shunji, Kobayashi, Shogo, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Loewenstein, Michael, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Mernier, François, Miller, Eric D, Miller, Jon M, Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakajima, Hiroshi, Nakazawa, Kazuhiro, Ness, Jan-Uwe, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Shoji, Ogorzalek, Anna, Okajima, Takashi, Ota, Naomi, Paltani, Stephane, Petre, Robert, Plucinsky, Paul, Scott Porter, Frederick, Pottschmidt, Katja, Sato, Kosuke, Sato, Toshiki, Sawada, Makoto, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall, Suzuki, Hiromasa, Szymkowiak, Andrew, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Tashiro, Makoto, Terada, Yukikatsu, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi G, Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Vink, Jacco, Watanabe, Shin, Williams, Brian J, Yamada, Satoshi, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yoneyama, Tomokage, Yoshida, Tessei, Yukita, Mihoko, Zhuravleva, Irina, Wang, Q Daniel, Amano, Yuki, Tanaka, Kojiro, Narita, Takuto, Ohshiro, Yuken, Yoshimoto, Anje, Aoki, Yuma, Balakrishnan, Mayura
    Publications of the Astronomical Society of Japan 2025年2月  
    Sagittarius A East is a supernova remnant with a unique surrounding environment, as it is located in the immediate vicinity of the supermassive black hole at the Galactic center, Sagittarius A<inline-formula><tex-math id="TM0001" notation="LaTeX">$^{*}$</tex-math></inline-formula>. The X-ray emission of the remnant is suspected to show features of overionized plasma, which would require peculiar evolutionary paths. We report on the first observation of Sagittarius A East with the X-Ray Imaging and Spectroscopy Mission (XRISM). Equipped with a combination of a high-resolution microcalorimeter spectrometer and a large field-of-view CCD imager, we for the first time resolved the Fe XXV K-shell lines into fine structure lines and measured the forbidden-to-resonance intensity ratio to be <inline-formula><tex-math id="TM0002" notation="LaTeX">$1.39 \pm 0.12$</tex-math></inline-formula>, which strongly suggests the presence of overionized plasma. We obtained a reliable constraint on the ionization temperature just before the transition into the overionization state, of <inline-formula><tex-math id="TM0003" notation="LaTeX">$\gt\! 4\:$</tex-math></inline-formula>keV. The recombination timescale was constrained to be <inline-formula><tex-math id="TM0004" notation="LaTeX">$\lt\! 8 \times 10^{11} \:$</tex-math></inline-formula>cm<inline-formula><tex-math id="TM0005" notation="LaTeX">$^{-3}\:$</tex-math></inline-formula>s. The small velocity dispersion of <inline-formula><tex-math id="TM0006" notation="LaTeX">$109 \pm 6\:$</tex-math></inline-formula>km<inline-formula><tex-math id="TM0007" notation="LaTeX">$\:$</tex-math></inline-formula>s<inline-formula><tex-math id="TM0008" notation="LaTeX">$^{-1}$</tex-math></inline-formula> indicates a low Fe ion temperature <inline-formula><tex-math id="TM0009" notation="LaTeX">$\lt\! 8\:$</tex-math></inline-formula>keV and a small expansion velocity <inline-formula><tex-math id="TM0010" notation="LaTeX">$\lt\! 200\:$</tex-math></inline-formula>km<inline-formula><tex-math id="TM0011" notation="LaTeX">$\:$</tex-math></inline-formula>s<inline-formula><tex-math id="TM0012" notation="LaTeX">$^{-1}$</tex-math></inline-formula>. The high initial ionization temperature and small recombination timescale suggest that either rapid cooling of the plasma via adiabatic expansion from dense circumstellar material or intense photoionization by Sagittarius A<inline-formula><tex-math id="TM0013" notation="LaTeX">$^{*}$</tex-math></inline-formula> in the past may have triggered the overionization....
  • Xrism Collaboration, Audard, Marc, Awaki, Hisamitsu, Ballhausen, Ralf, Bamba, Aya, Behar, Ehud, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V., Corrales, Lia, Costantini, Elisa, Cumbee, Renata, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Eckert, Dominique, Enoto, Teruaki, Eguchi, Satoshi, Ezoe, Yuichiro, Foster, Adam, Fujimoto, Ryuichi, Fujita, Yutaka, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, García, Javier A., Gu, Liyi, Guainazzi, Matteo, Hagino, Kouichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Hornschemeier, Ann, Ichinohe, Yuto, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Timothy, Kara, Erin, Katsuda, Satoru, Kanemaru, Yoshiaki, Kelley, Richard, Kilbourne, Caroline, Kitamoto, Shunji, Kobayashi, Shogo, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Loewenstein, Michael, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Mernier, François, Miller, Eric D., Miller, Jon M., Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakajima, Hiroshi, Nakazawa, Kazuhiro, Ness, Jan-Uwe, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Shoji, Ogorzalek, Anna, Okajima, Takashi, Ota, Naomi, Paltani, Stephane, Petre, Robert, Plucinsky, Paul, Porter, Frederick Scott, Pottschmidt, Katja, Sato, Kosuke, Sato, Toshiki, Sawada, Makoto, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall, Suzuki, Hiromasa, Szymkowiak, Andrew, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Tashiro, Makoto, Terada, Yukikatsu, Terashima, Yuichi, Trigo, María Díaz, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi G., Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Vink, Jacco, Watanabe, Shin, Williams, Brian J., Yamada, Satoshi, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yoneyama, Tomokage, Yoshida, Tessei, Yukita, Mihoko, Zhuravleva, Irina, Kondo, Marie, Werner, Norbert, Plšek, Tomáš, Sun, Ming, Hosogi, Kokoro, Majumder, Anwesh
    Nature 2025年2月  
    Galaxy clusters contain vast amounts of hot ionized gas known as the intracluster medium (ICM). In relaxed cluster cores, the radiative cooling time of the ICM is shorter than the age of the cluster. However, the absence of line emission associated with cooling suggests heating mechanisms that offset the cooling, with feedback from active galactic nuclei (AGNs) being the most likely source1,2. Turbulence and bulk motions, such as the oscillating ('sloshing') motion of the core gas in the cluster potential well, have also been proposed as mechanisms for heat distribution from the outside of the core3,4. Here we present X-ray spectroscopic observations of the Centaurus galaxy cluster with the X-Ray Imaging and Spectroscopy Mission satellite. We find that the hot gas flows along the line of sight relative to the central galaxy, with velocities from 130 km s‑1 to 310 km s‑1 within about 30 kpc of the centre. This indicates bulk flow consistent with core gas sloshing. Although the bulk flow may prevent excessive accumulation of cooled gas at the centre, it could distribute the heat injected by the AGN and bring in thermal energy from the surrounding ICM. The velocity dispersion of the gas is found to be only ≲120 km s‑1 in the core, even within about 10 kpc of the AGN. This suggests that the influence of the AGN on the surrounding ICM motion is limited in the cluster....
  • Chamani M. Gunasekera, Peter A. M. van Hoof, Masahiro Tsujimoto, Gary J. Ferland
    Astronomy & Astrophysics 2025年2月  
  • Yuto Mochizuki, Masahiro Tsujimoto, Richard L. Kelley, Bert Vander Meulen, Teruaki Enoto, Yutaro Nagai, Chris Done, Pragati Pradhan, Natalie Hell, Katja Pottschmidt, Ken Ebisawa, Ehud Behar
    The Astrophysical Journal Letters 2024年12月10日  
  • Xrism Collaboration, Audard, Marc, Awaki, Hisamitsu, Ballhausen, Ralf, Bamba, Aya, Behar, Ehud, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V., Corrales, Lia, Costantini, Elisa, Cumbee, Renata, Díaz Trigo, María, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Eckert, Dominique, Eguchi, Satoshi, Enoto, Teruaki, Ezoe, Yuichiro, Foster, Adam, Fujimoto, Ryuichi, Fujita, Yutaka, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, García, Javier A., Gu, Liyi, Guainazzi, Matteo, Hagino, Kouichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Hornschemeier, Ann, Ichinohe, Yuto, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Timothy, Kara, Erin, Katsuda, Satoru, Kanemaru, Yoshiaki, Kelley, Richard, Kilbourne, Caroline, Kitamoto, Shunji, Kobayashi, Shogo, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Loewenstein, Michael, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Mernier, François, Miller, Eric D., Miller, Jon M., Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakajima, Hiroshi, Nakazawa, Kazuhiro, Ness, Jan-Uwe, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Shoji, Ogorzalek, Anna, Okajima, Takashi, Ota, Naomi, Paltani, Stephane, Petre, Robert, Plucinsky, Paul, Porter, Frederick S., Pottschmidt, Katja, Sato, Kosuke, Sato, Toshiki, Sawada, Makoto, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall, Suzuki, Hiromasa, Szymkowiak, Andrew, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Tashiro, Makoto, Terada, Yukikatsu, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Vink, Jacco, Watanabe, Shin, Williams, Brian J., Yamada, Satoshi, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yoneyama, Tomokage, Yoshida, Tessei, Yukita, Mihoko, Zhuravleva, Irina, Tomaru, Ryota, Hayashi, Tasuku, Hakamata, Tomohiro, Miura, Daiki, Koljonen, Karri, McCollough, Mike
    The Astrophysical Journal 2024年12月  
    The X-ray binary system Cygnus X-3 (4U 2030+40, V1521 Cyg) is luminous but enigmatic owing to the high intervening absorption. High-resolution X-ray spectroscopy uniquely probes the dynamics of the photoionized gas in the system. In this Letter, we report on an observation of Cyg X-3 with the XRISM/Resolve spectrometer, which provides unprecedented spectral resolution and sensitivity in the 2–10 keV band. We detect multiple kinematic and ionization components in absorption and emission whose superposition leads to complex line profiles, including strong P Cygni profiles on resonance lines. The prominent Fe XXV Heα and Fe XXVI Lyα emission complexes are clearly resolved into their characteristic fine-structure transitions. Self-consistent photoionization modeling allows us to disentangle the absorption and emission components and measure the Doppler velocity of these components as a function of binary orbital phase. We find a significantly higher velocity amplitude for the emission lines than for the absorption lines. The absorption lines generally appear blueshifted by ∼‑500–600 km s‑1. We show that the wind decomposes naturally into a relatively smooth and large-scale component, perhaps associated with the background wind itself, plus a turbulent, denser structure located close to the compact object in its orbit....
  • Pradhan, P., Tsujimoto, M.
    Bulletin de la Societe Royale des Sciences de Liege 2024年12月  
    The X-ray Imaging and Spectrometer Mission (XRISM) was put into orbit successfully in September 2023. Resolve, one of the scientific instruments onboard XRISM, hosts an X-ray spectrometer based on X-ray microcalorimetery technology. It excels in high spectral resolution, a large throughput, a large bandpass, low background, and good timing accuracy. These properties are suited to bring new insights especially in high-mass X-ray binaries (HMXB). We describe these unique features of Resolve and present initial highlights of two HMXB sources....
  • XRISM Collaboration, Audard, Marc, Awaki, Hisamitsu, Ballhausen, Ralf, Bamba, Aya, Behar, Ehud, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V., Corrales, Lia, Costantini, Elisa, Cumbee, Renata, Diaz-Trigo, Maria, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan, Eckert, Dominique, Enoto, Teruaki, Eguchi, Satoshi, Ezoe, Yuichiro, Foster, Adam, Fujimoto, Ryuichi, Fujita, Yutaka, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, García, Javier A., Gu, Liyi, Guainazzi, Matteo, Hagino, Kouichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Hornschemeier, Ann, Ichinohe, Yuto, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Timothy, Kara, Erin, Katsuda, Satoru, Kanemaru, Yoshiaki, Kelley, Richard, Kilbourne, Caroline, Kitamoto, Shunji, Kobayashi, Shogo, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Loewenstein, Michael, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Mernier, François, Miller, Eric D., Miller, Jon M., Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakajima, Hiroshi, Nakazawa, Kazuhiro, Ness, Jan-Uwe, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Shoji, Ogorzalek, Anna, Okajima, Takashi, Ota, Naomi, Paltani, Stephane, Petre, Robert, Plucinsky, Paul, Porter, Frederick Scott, Pottschmidt, Katja, Sato, Kosuke, Sato, Toshiki, Sawada, Makoto, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall, Suzuki, Hiromasa, Szymkowiak, Andrew, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Tashiro, Makoto, Terada, Yukikatsu, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi G., Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Vink, Jacco, Watanabe, Shin, Williams, Brian J., Yamada, Satoshi, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yoneyama, Tomokage, Yoshida, Tessei, Yukita, Mihoko, Zhuravleva, Irina, Agarwal, Manan, Ohshiro, Yuken
    Publications of the Astronomical Society of Japan 2024年12月  
    We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N 132D in the Large Magellanic Cloud. The Resolve microcalorimeter has obtained the first high-resolution spectrum in the 1.6-10 keV band, which contains K-shell emission lines of Si, S, Ar, Ca, and Fe. We find that the Si and S lines are relatively narrow, with a broadening represented by a Gaussian-like velocity dispersion of <inline-formula><tex-math id="TM0001" notation="LaTeX">$\sigma _v \sim 450$</tex-math></inline-formula> km s<inline-formula><tex-math id="TM0002" notation="LaTeX">$^{-1}$</tex-math></inline-formula>. However, the Fe He<inline-formula><tex-math id="TM0003" notation="LaTeX">$\alpha$</tex-math></inline-formula> lines are substantially broadened with <inline-formula><tex-math id="TM0004" notation="LaTeX">$\sigma _v \sim 1670$</tex-math></inline-formula> km s<inline-formula><tex-math id="TM0005" notation="LaTeX">$^{-1}$</tex-math></inline-formula>. This broadening can be explained by a combination of the thermal Doppler effect due to the high ion temperature and the kinematic Doppler effect due to the SNR expansion. Assuming that the Fe He<inline-formula><tex-math id="TM0006" notation="LaTeX">$\alpha$</tex-math></inline-formula> emission originates predominantly from the supernova ejecta, we estimate the reverse shock velocity at the time when the bulk of the Fe ejecta were shock heated to be <inline-formula><tex-math id="TM0007" notation="LaTeX">$-1000 \lesssim V_{\rm rs}$</tex-math></inline-formula> (km s<inline-formula><tex-math id="TM0008" notation="LaTeX">$^{-1}$</tex-math></inline-formula>) <inline-formula><tex-math id="TM0009" notation="LaTeX">$\lesssim 3300$</tex-math></inline-formula> (in the observer frame). We also find that Fe Ly<inline-formula><tex-math id="TM0010" notation="LaTeX">$\alpha$</tex-math></inline-formula> emission is redshifted with a bulk velocity of <inline-formula><tex-math id="TM0011" notation="LaTeX">$\sim 890$</tex-math></inline-formula> km s<inline-formula><tex-math id="TM0012" notation="LaTeX">$^{-1}$</tex-math></inline-formula>, substantially larger than the radial velocity of the local interstellar medium surrounding N 132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs....
  • Yoshitomo Maeda, Ryuichi Fujimoto, Hisamitsu Awaki, Jesus C. Balleza, Kim R. Barnstable, Thomas G. Bialas, Rozenn Boissay-Malaquin, Gregory V. Brown, Edgar R. Canavan, Timothy M. Carnahan, Meng P. Chiao, Brian J. Comber, Elisa Costantini, Renata S. Cumbee, Jan-Willem A. den Herder, Johannes Dercksen, Cor P. de Vries, Michael J. DiPirro, Megan E. Eckart, Yuichiro Ezoe, Carlo Ferrigno, Nathalie Q. S. Gorter, Steven M. Graham, Martin Grim, Leslie S. Hartz, Ryota Hayakawa, Takayuki Hayashi, Natalie Hell, Akio Hoshino, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Bryan L. James, Yoshiaki Kanemaru, Richard L. Kelley, Steven J. Kenyon, Caroline A. Kilbourne, Mark O. Kimball, Shunji Kitamoto, Maurice A. Leutenegger, Dan McCammon, Brian J. McLaughlin, Joseph J. Miko, Erik van der Meer, Misaki Mizumoto, Takashi Okajima, Atsushi Okamoto, Stéphane Paltani, Frederick S. Porter, Lillian S. Reichenthal, Kosuke Sato, Toshiki Sato, Yohichi Sato, Makoto Sawada, Keisuke Shinozaki, Russell F. Shipman, Peter J. Shirron, Gary A. Sneiderman, Soong Yang, Richard Szymkiewicz, Andrew E. Szymkowiak, Yoh Takei, Mai Takeo, Tsubasa Tamba, Keisuke Tamura, Masahiro Tsujimoto, Yuusuke Uchida, Stephen Wasserzug, Michael C. Witthoeft, Rob Wolfs, Shinya Yamada, Susumu Yasuda
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 53-53 2024年8月22日  
  • Richard L. Kelley, Hisamitsu Awaki, Jesus C. Balleza, Kim R. Barnstable, Thomas G. Bialas, Rozenn Boissay-Malaquin, Gregory V. Brown, Edgar R. Canavan, Timothy M. Carnahan, Meng P. Chiao, Brian J. Comber, Elisa Costantini, Renata S. Cumbee, Jan-Willem A. den Herder, Johannes Dercksen, Cor de Vries, Michael J. DiPirro, Megan E. Eckart, Yuichiro Ezoe, Carlo Ferrigno, Ryuichi Fujimoto, Nathalie Q. S. Gorter, Steven M. Graham, Martin Grim, Leslie S. Hartz, Ryota Hayakawa, Takayuki Hayashi, Natalie Hell, Akio Hoshino, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Bryan L. James, Yoshiaki Kanemaru, Steven J. Kenyon, Caroline A. Kilbourne, Mark O. Kimball, Shunji Kitamoto, Maurice A. Leutenegger, Yoshitomo Maeda, Dan McCammon, Brian J. McLaughlin, Joseph J. Miko, Erik van der Meer, Misaki Mizumoto, Takashi Okajima, Atsushi Okamoto, Stéphane Paltani, Frederick S. Porter, Lillian S. Reichenthal, Kosuke Sato, Toshiki Sato, Yohichi Sato, Makoto Sawada, Keisuke Shinozaki, Russell F. Shipman, Peter J. Shirron, Gary A. Sneiderman, Soong Yang, Richard Szymkiewicz, Andrew E. Szymkowiak, Yoh Takei, Mai Takeo, Tsubasa Tamba, Keisuke Tamura, Masahiro Tsujimoto, Yuusuke Uchida, Stephen Wasserzug, Michael C. Witthoeft, Rob Wolfs, Shinya Yamada, Susumu Yasuda
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 55-55 2024年8月22日  
  • Frederick S. Porter, Caroline A. Kilbourne, Meng P. Chiao, Renata S. Cumbee, Megan E. Eckart, Ryuichi Fujimoto, Yoshitaka Ishisaki, Yoshiaki Kanemaru, Richard L. Kelley, Maurice A. Leutenegger, Yoshitomo Maeda, Misaki Mizumoto, Kosuke Sato, Makoto Sawada, Gary A. Sneiderman, Yoh Takei, Masahiro Tsujimoto, Yuusuke Uchida, Tomomi Watanabe, Shinya Yamada
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 56-56 2024年8月21日  
  • Takayuki Hayashi, Rozenn Boissay-Malaquin, Keisuke Tamura, Takashi Okajima, Megan E. Eckart, Maurice A. Leutenegger, Tahir Yaqoob, Michael Loewenstein, Richard L. Kelley, Frederick S. Porter, Caroline A. Kilbourne, Meng P. Chiao, Gary A. Sneiderman, Renata S. Cumbee, Yoshitaka Ishisaki, Ryuichi Fujimoto, Masahiro Tsujimoto, Makoto Sawada, Toshiki Sato, Yoshitomo Maeda, Manabu Ishida, Lia Corrales, Eric Miller, Aysegul Tumer, Hiromitsu Takahashi, Laura Brenneman, Yoshiaki Kanemaru, Misaki Mizumoto, Maxim Markevitch, Matteo Guainazzi
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 58-58 2024年8月21日  
  • Megan E. Eckart, Gregory V. Brown, Meng P. Chiao, Renata S. Cumbee, Ryuichi Fujimoto, Natalie Hell, Akio Hoshino, Yoshitaka Ishisaki, Richard L. Kelley, Steven J. Kenyon, Caroline A. Kilbourne, Shunji Kitamoto, Maurice A. Leutenegger, Thomas E. Lockard, Michael Loewenstein, Edward W. Magee, Misaki Mizumoto, Frederick S. Porter, Kosuke Sato, Makoto Sawada, Chintan D. Shah, Russell F. Shipman, Gary A. Sneiderman, Yoh Takei, Masahiro Tsujimoto, Cor P. de Vries, Tomomi Watanabe, Michael C. Witthoeft, Rob Wolfs, Shinya Yamada, Tahir Yaqoob
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 62-62 2024年8月21日  
  • Russell F. Shipman, Shunji Kitamoto, Rob Wolfs, Elisa Costantini, Megan E. Eckart, Carlo Ferrigno, Ludovic Genolet, Nathalie Q. S. Gorter, Martin Grim, Jan-Willem A. den Herder, Caroline A. Kilbourne, Maurice A. Leutenegger, Erik van der Meer, Misaki Mizumoto, Frederick S. Porter, Stéphane Paltani, Makoto Sawada, Simon Strotmann, Masahiro Tsujimoto, Cor P. de Vries
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 225-225 2024年8月21日  
  • Yuto Mochizuki, Masahiro Tsujimoto, Caroline A. Kilbourne, Megan E. Eckart, Yoshitaka Ishisaki, Yoshiaki Kanemaru, Maurice . Leutenegger, Misaki Mizumoto, Frederick S. Porter, Kosuke Sato, Makoto Sawada, Shinya Yamada
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 233-233 2024年8月21日  
  • Makoto Sawada, Renata S. Cumbee, Cor de Vries, Megan E. Eckart, Ryuichi Fujimoto, Yoshitaka Ishisaki, Caroline A. Kilbourne, Shunji Kitamoto, Maurice A. Leutenegger, Frederick S. Porter, Russell F. Shipman, Yoh Takei, Masahiro Tsujimoto
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 234-234 2024年8月21日  
  • Bert Vander Meulen, Peter Camps, Masahiro Tsujimoto, Keiichi Wada
    Astronomy & Astrophysics 2024年8月  
  • Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
    The Astrophysical Journal Letters 2024年7月1日  
  • Miki Kurihara, Wataru Buz Iwakiri, Masahiro Tsujimoto, Ken Ebisawa, Shin Toriumi, Shinsuke Imada, Yohko Tsuboi, Kazuki Usui, Keith C. Gendreau, Zaven Arzoumanian
    The Astrophysical Journal 965(2) 135-135 2024年4月1日  査読有り
  • Masahiro Tsujimoto
    Astrophysical Journal Letters 2024年  
  • Masahiro Tsujimoto
    Publications of the Astronomical Society of Japan 2024年  
  • Masahiro Tsujimoto
    ArXiv 2024年  
  • Masahiro Tsujimoto, Misaki Mizumoto, Ken Ebisawa, Hirokazu Odaka, Qazuya Wada
    Astrophysical Journal 960(1) 2024年1月1日  
  • Mayu Tominaga, Masahiro Tsujimoto, Ken Ebisawa, Teruaki Enoto, Kimitake Hayasaki
    Astrophysical Journal 958(1) 2023年11月1日  
  • R. Imamura, H. Awaki, M. Tsujimoto, S. Yamada, F. S. Porter, C. A. Kilbourne, R. L. Kelley, Y. Takei
    Journal of Low Temperature Physics 211(5-6) 426-433 2023年6月  
  • Tomoki Omama, Masahiro Tsujimoto, Ken Ebisawa, Misaki Mizumoto
    Astrophysical Journal 945(2) 2023年3月1日  
  • Masahiro Tsujimoto, Takayuki Hayashi, Kumiko Morihana, Yuki Moritani
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 75(1) 177-186 2023年2月  
  • Miki Kurihara, Masahiro Tsujimoto, Megan E. Eckart, Caroline A. Kilbourne, Frederick T. Matsuda, Brian Mclaughlin, Shugo Oguri, Frederick S. Porter, Yoh Takei, Yoichi Kochibe
    Journal of Astronomical Telescopes, Instruments, and Systems 9(1) 18004 2023年1月1日  
  • Takashi Hasebe, Ryuta Imamura, Masahiro Tsujimoto, Hisamitsu Awaki, Meng P. Chiao, Ryuichi Fujimoto, Leslie S. Hartz, Caroline A. Kilbourne, Gary A. Sneiderman, Yoh Takei, Susumu Yasuda
    Journal of Astronomical Telescopes, Instruments, and Systems 9(1) 14003 2023年1月1日  
  • T. Hasebe, P. A. R. Ade, A. Adler, E. Allys, D. Alonso, K. Arnold, D. Auguste, J. Aumont, R. Aurlien, J. Austermann, S. Azzoni, C. Baccigalupi, A. J. Banday, R. Banerji, R. B. Barreiro, N. Bartolo, S. Basak, E. Battistelli, L. Bautista, J. Beall, D. Beck, S. Beckman, K. Benabed, J. Bermejo-Ballesteros, M. Bersanelli, J. Bonis, J. Borrill, F. Bouchet, F. Boulanger, S. Bounissou, M. Brilenkov, M. L. Brown, M. Bucher, E. Calabrese, M. Calvo, P. Campeti, A. Carones, F. J. Casas, A. Catalano, A. Challinor, V. Chan, K. Cheung, Y. Chinone, J. Cliche, F. Columbro, W. Coulton, J. Cubas, A. Cukierman, D. Curtis, G. D’Alessandro, K. Dachlythra, P. de Bernardis, T. de Haan, E. de la Hoz, M. De Petris, S. Della Torre, C. Dickinson, P. Diego-Palazuelos, M. Dobbs, T. Dotani, D. Douillet, L. Duband, A. Ducout, S. Duff, J. M. Duval, K. Ebisawa, T. Elleflot, H. K. Eriksen, J. Errard, T. Essinger-Hileman, F. Finelli, R. Flauger, C. Franceschet, U. Fuskeland, S. Galli, M. Galloway, K. Ganga, J. R. Gao, R. T. Genova-Santos, M. Gerbino, M. Gervasi, T. Ghigna, S. Giardiello, E. Gjerløw, M. L. Gradziel, J. Grain, L. Grandsire, F. Grupp, A. Gruppuso, J. E. Gudmundsson, N. W. Halverson, J. Hamilton, P. Hargrave, M. Hasegawa, M. Hattori, M. Hazumi, S. Henrot-Versillé, L. T. Hergt, D. Herman, D. Herranz, C. A. Hill, G. Hilton, E. Hivon, R. A. Hlozek, T. D. Hoang, A. L. Hornsby, Y. Hoshino, J. Hubmayr, K. Ichiki, T. Iida, H. Imada, K. Ishimura, H. Ishino, G. Jaehnig, M. Jones, T. Kaga, S. Kashima, N. Katayama, A. Kato, T. Kawasaki, R. Keskitalo, T. Kisner, Y. Kobayashi, N. Kogiso, A. Kogut, K. Kohri, E. Komatsu, K. Komatsu, K. Konishi, N. Krachmalnicoff, I. Kreykenbohm, C. L. Kuo, A. Kushino, L. Lamagna, J. V. Lanen, G. Laquaniello, M. Lattanzi, A. T. Lee, C. Leloup, F. Levrier, E. Linder, T. Louis, G. Luzzi, J. Macias-Perez, T. Maciaszek, B. Maffei, D. Maino, M. Maki, S. Mandelli, M. Maris, E. Martínez-González, S. Masi, M. Massa, S. Matarrese, F. T. Matsuda, T. Matsumura, L. Mele, A. Mennella, M. Migliaccio, Y. Minami, K. Mitsuda, A. Moggi, A. Monfardini, J. Montgomery, L. Montier, G. Morgante, B. Mot, Y. Murata, J. A. Murphy, M. Nagai, Y. Nagano, T. Nagasaki, R. Nagata, S. Nakamura, R. Nakano, T. Namikawa, F. Nati, P. Natoli, S. Nerval, T. Nishibori, H. Nishino, F. Noviello, C. O’Sullivan, K. Odagiri, H. Ogawa, H. Ogawa, S. Oguri, H. Ohsaki, I. S. Ohta, N. Okada, N. Okada, L. Pagano, A. Paiella, D. Paoletti, A. Passerini, G. Patanchon, V. Pelgrim, J. Peloton, F. Piacentini, M. Piat, G. Pisano, G. Polenta, D. Poletti, T. Prouvé, G. Puglisi, D. Rambaud, C. Raum, S. Realini, M. Reinecke, M. Remazeilles, A. Ritacco, G. Roudil, J. Rubino-Martin, M. Russell, H. Sakurai, Y. Sakurai, M. Sandri, M. Sasaki, G. Savini, D. Scott, J. Seibert, Y. Sekimoto, B. Sherwin, K. Shinozaki, M. Shiraishi, P. Shirron, G. Signorelli, G. Smecher, F. Spinella, S. Stever, R. Stompor, S. Sugiyama, R. Sullivan, A. Suzuki, J. Suzuki, T. L. Svalheim, E. Switzer, R. Takaku, H. Takakura, S. Takakura, Y. Takase, Y. Takeda, A. Tartari, D. Tavagnacco, A. Taylor, E. Taylor, Y. Terao, J. Thermeau, H. Thommesen, K. L. Thompson, B. Thorne, T. Toda, M. Tomasi, M. Tominaga, N. Trappe, M. Tristram, M. Tsuji, M. Tsujimoto, C. Tucker, J. Ullom, L. Vacher, G. Vermeulen, P. Vielva, F. Villa, M. Vissers, N. Vittorio, B. Wandelt, W. Wang, K. Watanuki, I. K. Wehus, J. Weller, B. Westbrook, J. Wilms, B. Winter, E. J. Wollack, N. Y. Yamasaki, T. Yoshida, J. Yumoto, A. Zacchei, M. Zannoni, A. Zonca
    Journal of Low Temperature Physics 211(5-6) 384-397 2022年12月2日  
  • M. Tsuji, M. Tsujimoto, Y. Sekimoto, T. Dotani, M. Shiraishi
    Journal of Low Temperature Physics 209(5-6) 1097-1103 2022年12月  
  • E Allys, K Arnold, J Aumont, R Aurlien, S Azzoni, C Baccigalupi, A J Banday, R Banerji, R B Barreiro, N Bartolo, L Bautista, D Beck, S Beckman, M Bersanelli, F Boulanger, M Brilenkov, M Bucher, E Calabrese, P Campeti, A Carones, F J Casas, A Catalano, V Chan, K Cheung, Y Chinone, S E Clark, F Columbro, G D’Alessandro, P de Bernardis, T de Haan, E de  la Hoz, M De Petris, S Della Torre, P Diego-Palazuelos, M Dobbs, T Dotani, J M Duval, T Elleflot, H K Eriksen, J Errard, T Essinger-Hileman, F Finelli, R Flauger, C Franceschet, U Fuskeland, M Galloway, K Ganga, M Gerbino, M Gervasi, R T Génova-Santos, T Ghigna, S Giardiello, E Gjerløw, J Grain, F Grupp, A Gruppuso, J E Gudmundsson, N W Halverson, P Hargrave, T Hasebe, M Hasegawa, M Hazumi, S Henrot-Versillé, B Hensley, L T Hergt, D Herman, E Hivon, R A Hlozek, A L Hornsby, Y Hoshino, J Hubmayr, K Ichiki, T Iida, H Imada, H Ishino, G Jaehnig, N Katayama, A Kato, R Keskitalo, T Kisner, Y Kobayashi, A Kogut, K Kohri, E Komatsu, K Komatsu, K Konishi, N Krachmalnicoff, C L Kuo, L Lamagna, M Lattanzi, A T Lee, C Leloup, F Levrier, E Linder, G Luzzi, J Macias-Perez, T Maciaszek, B Maffei, D Maino, S Mandelli, E Martínez-González, S Masi, M Massa, S Matarrese, F T Matsuda, T Matsumura, L Mele, M Migliaccio, Y Minami, A Moggi, J Montgomery, L Montier, G Morgante, B Mot, Y Nagano, T Nagasaki, R Nagata, R Nakano, T Namikawa, F Nati, P Natoli, S Nerval, F Noviello, K Odagiri, S Oguri, H Ohsaki, L Pagano, A Paiella, D Paoletti, A Passerini, G Patanchon, F Piacentini, M Piat, G Polenta, D Poletti, T Prouvé, G Puglisi, D Rambaud, C Raum, S Realini, M Reinecke, M Remazeilles, A Ritacco, G Roudil, J A Rubino-Martin, M Russell, H Sakurai, Y Sakurai, M Sasaki, D Scott, Y Sekimoto, K Shinozaki, M Shiraishi, P Shirron, G Signorelli, F Spinella, S Stever, R Stompor, S Sugiyama, R M Sullivan, A Suzuki, T L Svalheim, E Switzer, R Takaku, H Takakura, Y Takase, A Tartari, Y Terao, J Thermeau, H Thommesen, K L Thompson, M Tomasi, M Tominaga, M Tristram, M Tsuji, M Tsujimoto, L Vacher, P Vielva, N Vittorio, W Wang, K Watanuki, I K Wehus, J Weller, B Westbrook, J Wilms, E J Wollack, J Yumoto, M Zannoni
    Progress of Theoretical and Experimental Physics 2023(4) 2022年11月21日  
  • J. Hubmayr, P. A.R. Ade, A. Adler, E. Allys, D. Alonso, K. Arnold, D. Auguste, J. Aumont, R. Aurlien, J. E. Austermann, S. Azzoni, C. Baccigalupi, A. J. Banday, R. Banerji, R. B. Barreiro, N. Bartolo, S. Basak, E. Battistelli, L. Bautista, J. A. Beall, D. Beck, S. Beckman, K. Benabed, J. Bermejo-Ballesteros, M. Bersanelli, J. Bonis, J. Borrill, F. Bouchet, F. Boulanger, S. Bounissou, M. Brilenkov, M. L. Brown, M. Bucher, E. Calabrese, M. Calvo, P. Campeti, A. Carones, F. J. Casas, A. Catalano, A. Challinor, V. Chan, K. Cheung, Y. Chinone, C. Chiocchetta, S. E. Clark, L. Clermont, S. Clesse, J. Cliche, F. Columbro, J. A. Connors, A. Coppolecchia, W. Coulton, J. Cubas, A. Cukierman, D. Curtis, F. Cuttaia, G. D’Alessandro, K. Dachlythra, P. de Bernardis, T. de Haan, E. de la Hoz, M. De Petris, S. Della Torre, J. J. Daz Garca, C. Dickinson, P. Diego-Palazuelos, M. Dobbs, T. Dotani, D. Douillet, E. Doumayrou, L. Duband, A. Ducout, S. M. Duff, J. M. Duval, K. Ebisawa, T. Elleflot, H. K. Eriksen, J. Errard, T. Essinger-Hileman, S. Farrens, F. Finelli, R. Flauger, K. Fleury-Frenette, C. Franceschet, U. Fuskeland, L. Galli, S. Galli, M. Galloway, K. Ganga, J. R. Gao, R. T. Genova-Santos, M. Georges, M. Gerbino, M. Gervasi, T. Ghigna, S. Giardiello, E. Gjerlw, R. Gonzlez Gonzles, M. L. Gradziel, J. Grain
    Journal of Low Temperature Physics 209(3-4) 396-408 2022年11月  
  • M. Tsuji, M. Tsujimoto, Y. Sekimoto, T. Dotani, M. Shiraishi
    JOURNAL OF LOW TEMPERATURE PHYSICS 2022年11月  
  • Mayu Tominaga, Masahiro Tsujimoto, Graeme Smecher, Hirokazu Ishino
    JOURNAL OF LOW TEMPERATURE PHYSICS 209(3-4) 686-692 2022年11月  
  • Morihana, K., Tsujimoto, M., Ebisawa, K., Gandhi, P.
    VizieR Online Data Catalog 2022年9月  
    A deep JHKs imaging observation of the Chandra bulge field (CBF) was carried out using MOIRCS on the Subaru telescope. MOIRCS is equipped with two 2048x2048 HgCdTe HAWAII-2 arrays and covers a 4x7-arcmin2 field of view with a pixel scale of 0.117"/pixel in the imaging mode. <P />We look for candidate NIR counterparts to the Chandra X-ray sources. <P />(1 data file)....
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MISC

 26
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  • 関本裕太郎, 堂谷忠靖, 篠崎慶亮, 高倉隼人, 辻本匡弘, 長谷部孝, 満田和久, 永田竜, 羽澄昌史, 南雄人, 片山伸彦, 桜井雄基, 菅井肇, 高倉理, 松村知岳, 石野宏和, 魚住聖, 鹿島伸悟, 小松英一郎, 今田大皓
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所属学協会

 2

共同研究・競争的資金等の研究課題

 7
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