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419 results on '"Fukushima, Kotaro"'

1. Seasonal variation in home blood pressure during pregnancy and frequency of hypertensive disorders of pregnancy: a multicenter prospective study of home blood pressure measurements in pregnant women using information technology

Author

Jwa, Seung Chik, Takano, Natsuko, Tamaru, Shunsuke, Kijima, Sachi, Uesato, Tadashi, Matsubara, Keiichi, Tanaka, Kanji, Doi, Koutarou, Sameshima, Hiroshi, Iriyama, Takayuki, Fukushima, Kotaro, Hirata, Yoshiyasu, Fujii, Tomoyuki, Ishiwata, Isamu, Kamei, Yoshimasa, and Seki, Hiroyuki

Published
2025
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2. The soft X-ray background with Suzaku II: Supervirial temperature bubbles?

Author

Sugiyama, Hayato, Ueda, Masaki, Fukushima, Kotaro, Kobayashi, Shogo B., Yamasaki, Noriko Y., Sato, Kosuke, and Matsushita, Kyoko

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Observations of the hot X-ray emitting interstellar medium in the Milky Way are important for studying the stellar feedback and understanding the formation and evolution of galaxies. We present measurements of the soft X-ray background emission for 130 Suzaku observations at $75^\circ15^\circ$. With the standard soft X-ray background model consisting of the local hot bubble and the Milky Way halo, residual structures remain at 0.7--1 keV in the spectra of some regions. Adding a collisional-ionization-equilibrium component with a temperature of $\sim$0.8 keV, much higher than the virial temperature of the Milky Way, significantly reduces the derived C-statistic for 56 out of 130 observations. The emission measure of the 0.8 keV component varies by more than an order of magnitude: Assuming the solar abundance, the median value is 3$\times 10^{-4}~ \rm{cm^{-6} pc}$ and the 16th-84th percentile range is (1--8)$\times 10^{-4}~ \rm{cm^{-6} pc}$. Regions toward the Orion-Eridanus Superbubble, a large cavity extending from the Ori OB1 association, have the highest emission measures of the 0.8 keV component. While the scatter is large, the emission measures tend to be higher toward the lower Galactic latitude. We discuss possible biases caused by the solar wind charge exchange, stars, and background groups. The 0.8 keV component is probably heated by supernovae in the Milky Way disk, possibly related to galactic fountains., Comment: 14 pages, 9 figures, PASJ in press

Published
2023

4. O, Ne, Mg, and Fe Abundances in Hot X-Ray-emitting Halos of Galaxy Clusters, Groups, and Giant Early-type Galaxies with XMM-Newton RGS Spectroscopy

Author

Fukushima, Kotaro, Kobayashi, Shogo B., and Matsushita, Kyoko

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Chemical elements in the hot medium permeating early-type galaxies, groups, and clusters make them an excellent laboratory for studying metal enrichment and cycling processes in the largest scales of the universe. Here, we report the analysis by the XMM-Newton Reflection Grating Spectrometer of 14 early-type galaxies, including the well-known brightest cluster galaxies of Perseus, for instance. The spatial distribution of the O/Fe, Ne/Fe, and Mg/Fe ratios is generally flat at the central 60 arcsecond regions of each object, irrespective of whether or not a central Fe abundance drop has been reported. Common profiles between noble gas and normal metal suggest that the dust depletion process does not work predominantly in these systems. Therefore, observed abundance drops are possibly attributed to other origins, like systematics in the atomic codes. Giant systems of high gas mass-to-luminosity ratio tend to hold a hot gas ($\sim$ 2 keV) yielding the solar N/Fe, O/Fe, Ne/Fe, Mg/Fe, and Ni/Fe ratios. Contrarily, light systems at a subkiloelectronvolt temperature regime, including isolated or group-centered galaxies, generally exhibit super-solar N/Fe, Ni/Fe, Ne/O, and Mg/O ratios. We find that the latest supernova nucleosynthesis models fail to reproduce such a super-solar abundance pattern. Possible systematic uncertainties contributing to these high abundance ratios of cool objects are also discussed in tandem with the crucial role of future X-ray missions., Comment: 18 pages, 10 figures, 5 tables. Corrected some typos and references. Accepted for publication in ApJ

Published
2023
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5. The soft X-ray background with Suzaku: I. Milky Way halo

Author

Ueda, Masaki, Sugiyama, Hayato, Kobayashi, Shogo B., Fukushima, Kotaro, Yamasaki, Noriko Y., Sato, Kosuke, and Matsushita, Kyoko

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present measurements of the soft X-ray background emission for 130 Suzaku observations at $75^\circ15^\circ$ obtained from 2005 to 2015, covering nearly one solar cycle. In addition to the standard soft X-ray background model consisting of the local hot bubble and the Milky Way Halo (MWH), we include a hot collisional-ionization-equilibrium component with a temperature of $\sim 0.8$ keV to reproduce spectra of a significant fraction of the lines of sight. Then, the scatter in the relation between the emission measure vs. temperature of the MWH component is reduced. Here, we exclude time ranges with high count rates to minimize the effect of the solar wind charge exchange (SWCX). However, the spectra of almost the same lines of sight are inconsistent. The heliospheric SWCX emissions likely contaminate and gives a bias in measurements of temperature and the emission measure of the MWH. Excluding the data around the solar maximum and using the data taken before the end of 2009, at $|b|>35^\circ$ and $105^\circ

Published
2022
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6. Chemical enrichment in the cool core of the Centaurus cluster of galaxies

Author

Fukushima, Kotaro, Kobayashi, Shogo B., and Matsushita, Kyoko

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Here we present results from over 500 kiloseconds Chandra and XMM-Newton observations of the cool core of the Centaurus cluster. We investigate the spatial distributions of the O, Mg, Si, S, Ar, Ca, Cr, Mn, Fe, and Ni abundances in the intracluster medium with CCD detectors, and those of N, O, Ne, Mg, Fe, and Ni with the Reflection Grating Spectrometer (RGS). The abundances of most of the elements show a sharp drop within the central 18 arcsec, although different detectors and atomic codes give significantly different values. The abundance ratios of the above elements, including Ne/Fe with RGS, show relatively flat radial distributions. In the innermost regions with the dominant Fe-L lines, the measurements of the absolute abundances are challenging. For example, AtomDB and SPEXACT give Fe = 0.5 and 1.4 solar, respectively, for the spectra from the innermost region. These results suggest some systematic uncertainties in the atomic data and response matrices at least partly cause the abundance drop rather than the metal depletion into the cold dust. Except for super-solar N/Fe and Ni/Fe, sub-solar Ne/Fe, and Mg/Fe, the abundance pattern agrees with the solar composition. The entire pattern is challenging to reproduce with the latest supernova nucleosynthesis models. Observed super-solar N/O and comparable Mg abundance to stellar metallicity profiles imply the mass-loss winds dominate the intracluster medium in the brightest cluster galaxy. The solar Cr/Fe and Mn/Fe ratios indicate a significant contribution of near- and sub-Chandrasekhar mass explosions of Type Ia supernovae., Comment: 18 pages, 13 figures. Accepted for publication in MNRAS

Published
2022
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7. Element Stratification in the Middle-Aged Type Ia Supernova Remnant G344.7-0.1

Author

Fukushima, Kotaro, Yamaguchi, Hiroya, Slane, Patrick O., Park, Sangwook, Katsuda, Satoru, Sano, Hidetoshi, Lopez, Laura A., Plucinsky, Paul P., Kobayashi, Shogo B., and Matsushita, Kyoko

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Despite their importance, a detailed understanding of Type Ia supernovae (SNe Ia) remains elusive. X-ray measurements of the element distributions in supernova remnants (SNRs) offer important clues for understanding the explosion and nucleosynthesis mechanisms for SNe Ia. However, it is challenging to observe the entire ejecta mass in X-rays for young SNRs, because the central ejecta may not have been heated by the reverse shock yet. Here we present over 200 kilosecond Chandra observations of the Type Ia SNR G344.7-0.1, whose age is old enough for the reverse shock to have reached the SNR center, providing an opportunity to investigate the distribution of the entire ejecta mass. We reveal a clear stratification of heavy elements with a centrally peaked distribution of the Fe ejecta surrounded by intermediate-mass elements (IMEs: Si, S, Ar Ca) with an arc-like structure. The centroid energy of the Fe K emission is marginally lower in the central Fe-rich region than in the outer IME-rich regions, suggesting that the Fe ejecta were shock-heated more recently. These results are consistent with the prediction for standard SN Ia models, where the heavier elements are synthesized in the interior of an exploding white dwarf. We find, however, that the peak location of the Fe K emission is slightly offset to the west with respect to the geometric center of the SNR. This apparent asymmetry is likely due to the inhomogeneous density distribution of the ambient medium, consistent with our radio observations of the ambient molecular and neutral gas., Comment: 16 pages, 10 figures, Accepted for publication in Astrophysical Journal

Published
2020
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10. Evaluation of the initial pointing accuracy of XRISM

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Kanemaru, Yoshiaki, Iizuka, Ryo, Maeda, Yoshitomo, Okajima, Takashi, Hayashi, Takayuki, Kiyokane, Kazuhiro, Nihei, Yuto, Kominato, Takashi, Ishida, Manabu, Natsukari, Chikara, Watanabe, Shin, Sato, Kosuke, Terada, Yukikatsu, Hayashi, Katsuhiro, Baluta, Chris, Yoshida, Tessei, Hoshino, Akio, Ogawa, Shoji, Fukushima, Kotaro, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Nakazawa, Kazuhiro, Uno, Shin'ichiro, Ebisawa, Ken, Eguchi, Satoshi, Katsuda, Satoru, Kubota, Aya, Ota, Naomi, Shidatsu, Megumi, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yuusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Tomokage, Yoneyama, Yamada, Satoshi, Uchida, Nagomi, Sato, Rie, Holland, Matt, Loewenstein, Michael, Miller, Eric, Yaqoob, Tahir, Hill, Robert, Doyle, Trisha, Perez-Solis, Efrain, Waddy, Morgan, Mekosh, Mark, Fox, Joseph, Tashiro, Makoto, Toda, Kenichi, and Maejima, Hironori

Published
2024
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11. Detail design of the XRISM timing system and its verification in the nominal operation mode

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Terada, Yukikatsu, Shidatsu, Megumi, Sawada, Makoto, Kominato, Takashi, Kato, So, Sato, Ryohei, Sakama, Minami, Shioiri, Takumi, Niida, Yuki, Natsukari, Chikara, Tashiro, Makoto S., Toda, Kenichi, Maejima, Hironori, Hayashi, Katsuhiro, Yoshida, Tessei, Ogawa, Shoji, Kanemaru, Yoshiaki, Hoshino, Akio, Fukushima, Kotaro, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Nakazawa, Kazuhiro, Uno, Shin'ichiro, Ebisawa, Ken, Eguchi, Satoshi, Katsuda, Satoru, Kubota, Aya, Ota, Naomi, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Yoneyama, Tomokage, Yamada, Satoshi, Uchida, Nagomi, Watanabe, Shin, Iizuka, Ryo, Sato, Rie, Baluta, Chris, Holland, Matt, Loewenstein, Michael, Miller, Eric D., Yaqoob, Tahir, Hill, Robert S., Doyle, Trisha F., Perez-Solis, Efrain, Waddy, Morgan D., Mekosh, Mark, Fox, Joseph B., Takagi, Toshihiro, Motogami, Yugo, Pottschmidt, Katja, Enoto, Teruaki, and Tanaka, Takaaki

Published
2024
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12. The in-orbit XRISM science operations

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Hayashi, Katsuhiro, Tashiro, Makoto, Terada, Yukikatsu, Yoshida, Tessei, Ogawa, Shoji, Kanemaru, Yoshiaki, Fukushima, Kotaro, Hoshino, Akio, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Nakazawa, Kazuhiro, Uno, Shin'ichiro, Ebisawa, Ken, Eguchi, Satoshi, Katsuda, Satoru, Kitaguchi, Takao, Kubota, Aya, Ota, Naomi, Shidatsu, Megumi, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yuusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Yoneyama, Tomokage, Yamada, Satoshi, Uchida, Nagomi, Sakurai, Seiko, Watanabe, Shin, Iizuka, Ryo, Sato, Rie, Baluta, Chris, Tamura, Takayuki, Fukazawa, Yasushi, Odaka, Hirokazu, Tamba, Tsubasa, Sato, Ryohei, Kato, Sou, Sakama, Minami, Shioiri, Takumi, Niida, Yuki, Sakamoto, Natsuki, Nemoto, Noboru, Omiya, Yuki, Suzuki, Nari, Takagi, Toshihiro, Motogami, Yugo, Holland, Matt, Loewenstein, Michael, Miller, Eric, Yaqoob, Tahir, Hill, Robert, Doyle, Trisha, Perez-Solis, Efrain, Waddy, Morgan, Mekosh, Mark, Fox, Joseph, Guainazzi, Matteo, Ness, Jan-Uwe, Maejima, Hironori, Toda, Ken'ichi, and Natsukari, Chikara

Published
2024
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13. Development and operation status of X-Ray Imaging and Spectroscopy Mission (XRISM)

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Tashiro, Makoto, Watanabe, Shin, Maejima, Hironori, Toda, Kenichi, Matsushita, Kyoko, Yamaguchi, Hiroya, Kelley, Richard, Reichenthal, Lillian, Hartz, Leslie, Petre, Robert, Williams, Brian, Guainazzi, Matteo, Santovincenzo, Andrea, Costantini, Elisa, Takei, Yoh, Ishisaki, Yoshitaka, Fujimoto, Ryuichi, Henegar-Leon, Joy, Sneiderman, Gary, Tomida, Hiroshi, Mori, Koji, Nakajima, Hiroshi, Terada, Yukikatsu, Holland, Matt, Loewenstein, Micheal, Kallman, Timothy, Kaastra, Jelle, Miller, Eric, Sawada, Makoto, Done, Chris, Enoto, Teruaki, Bamba, Aya, Plucinsky, Paul, Ueda, Yoshihiro, Kara, Erin, Zhuravleva, Irina, Fujita, Yutaka, Querro, Jose Antonio, Arai, Yoshitaka, Audard, Marc, Awaki, Hisamitsu, Baluta, Chris, Bando, Nobutaka, Behar, Ehud, Bialas, Thomas, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V., Chiao, Meng, Corrales, Lia, Cumbee, Renata, de Vries, Cor, den Herder, Jan-Willem, Diaz-Trigo, Maria, DiPirro, Michael, Dotani, Tadayasu, Ebrero Carrero, Jacobo, Ebisawa, Ken, Eckart, Megan, Eckart, Dominique, Eguchi, Satoshi, Ezoe, Yuichiro, Ferrigno, Carlo, Foster, Adam, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, Gorter, Nathalie, Grim, Martin, Gu, Liyi, Hagino, Koichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Horiuchi, Takafumi, Hornschemeier, Ann, Hoshino, Akio, Ichinohe, Yuto, Ikuta, Chisato, Iizuka, Ryo, Ishi, Daiki, Ishida, Manabu, Ishihama, Naoki, Ishikawa, Kumi, Ishimura, Kosei, Jaffe, Tess, Katsuda, Satoru, Kanemaru, Yoshiaki, Kenyon, Steven, Kilbourne, Caroline, Kimball, Mark, Kitamoto, Shunji, Kobayashi, Shogo, Kobayashi, Akihide, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Li, Muzi, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsuzaki, Keiichi, McCammon, Dan, McLaughlin, Brian, McNamara, Brian, Miko, Joseph, Miller, Jon, Minesugi, Kenji, Mitani, Shinji, Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakazawa, Kazuhiro, Natsukari, Chikara, Ness, Jan-Uwe, Nigo, Kenichiro, Nishiyama, Mari, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Mina, Ogawa, Shoji, Okajima, Takashi, Okamoto, Atsushi, Ota, Naomi, Ozaki, Masanobu, Paltani, Stephane, Porter, F. Scott, Pottschmidt, Katja, Sasaki, Takahiro, Sato, Kosuke, Sato, Rie, Sato, Toshiki, Sato, Yoichi, Seta, Hiromi, Shida, Maki, Shidatsu, Megumi, Shigeto, Shuhei, Shipman, Russel, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Smith, Randall, Soong, Yang, Suzuki, Hiromasa, Szymkowiak, Andy, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Uno, Shinichiro, Van der Meer, Erik, Vink, Jacco, Wittheof, Michael, Wolfs, Rob, Yamada, Satoshi, Yamada, Shinya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yanagase, Keiichi, Yaqoob, Tahir, Yasuda, Susumu, Yoneyama, Tomokage, and Yoshida, Tessei

Published
2024
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14. Basic characteristics of Vision badge and its performance as an eye lens dosimeter for endoscopists.

Author

Fukushima, Kotaro, Matsubara, Kosuke, and Ichikawa, Nao

Subjects
*CRYSTALLINE lens, *OPTICALLY stimulated luminescence, *DOSIMETERS, *VISION, *BADGES
Abstract

Vision badge is an eye lens dosimeter to measure H p(3). This study aimed to evaluate the basic characteristics of the Vision badge and its performance as an eye lens dosimeter for endoscopists by phantom study. Energy dependence was evaluated by changing the tube voltage to 50 kV (effective energy of 27.9 keV), 80 kV (32.2 keV), and 120 kV (38.7 keV). Dose linearity was evaluated by changing the number of irradiation to 1, 5, and 40 times, which corresponded to 0.53, 5.32, and 21.4 mGy. Batch uniformity was evaluated by calculating the coefficient of variation of H p(3) obtained from 10 Vision badges. Angular dependence was evaluated at 0° (perpendicular to the incident direction of x-rays), 30°, 60°, 75°, and 90°. The Vision badge and optically stimulated luminescence (OSL) dosimeter were attached to the inside of the radioprotective glasses, worn on the endoscopist phantom, and the H p(3) obtained from both dosimeters were compared. The H p(3) obtained from the Vision badge with 38.7 keV was 3.8% higher than that with 27.9 keV. The Vision badge showed excellent linearity (R 2 = 1.00) with the air kerma up to 21.4 mGy. The coefficient of variation of the H p(3) for 10 Vision badges was 3.47%. The relative dose of the Vision badge decreased as the angle increased up to 75°, but increased at 90°. The H p(3) obtained by the OSL dosimeter and the Vision badge were decreased as the endoscopist phantom was turned away from the patient phantom. The H p(3) that was obtained by the Vision badge was 35.5%–55.0% less than that obtained by the nanoDot. In conclusion, the Vision badge showed specific angular dependence due to its shape, but satisfactory basic properties were exhibited for all characteristics. In phantom study, the Vision badge showed generally similar trends with the OSL dosimeter. [ABSTRACT FROM AUTHOR]

Published
2024
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18. 第79回日本放射線技術学会 総会学術大会 学生会員派遣報告

Author

Kobayashi, Daiki, primary, Nishigami, Rina, additional, Fukushima, Kotaro, additional, Tateishi, Masaru, additional, Seo, Tomoyuki, additional, Hizukuri, Kyoko, additional, Koda, Riku, additional, Kita, Kento, additional, Dang Quoc, Soai, additional, Mitsushima, Kazuki, additional, Kodama, Takumi, additional, Kumamoto, Jintaro, additional, Kotani, Hina, additional, and Oshiro, Tomotaka, additional

Published
2023
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21. Guidelines for obstetrical practice in Japan: Japan Society of Obstetrics and Gynecology and Japan Association of Obstetricians and Gynecologists 2020 edition

Author

Atsuo Itakura, Satoh Shoji, Aoki Shigeru, Fukushima Kotaro, Hasegawa Junichi, Hyodo Hironobu, Yoshimasa Kamei, Kondoh Eiji, Makino Shintaro, Matsuoka Ryu, Morikawa Mamoru, Nagamatsu Takeshi, Nakata Masahiko, Katsuhiko Naruse, Nishigori Hidekazu, Nishiguchi Tomizo, Obata‐Yasuoka Mana, Ohno Yasumasa, Oura Kuniaki, Shimoya Koichiro, Shiozaki Arihiro, Suzuki Shunji, Tanaka Kanji, Yoshida Shiro, Kudo Yoshiki, Maeda Tsugio, and Shozu Makio

Subjects
Obstetrics and Gynecology
Abstract

The 2017 clinical guidelines for obstetrical practice by the Japan Society of Obstetrics and Gynecology and the Japan Association of Obstetricians and Gynecologists were revised and published as the 2020 edition (in Japanese). The aim of these guidelines is to present appropriate standard obstetric diagnosis and management procedures that have reached consensus among Japanese obstetricians. The 2020 guidelines include 113 clinical questions and an appendix, followed by answers (CQA; originally 112 in the 2017 edition), a discussion, list of references, and some tables and figures presenting common problems and questions encountered in obstetrical practice. Each answer comes with a recommendation level of A, B, or C and has been prepared based principally on evidence or a consensus among Japanese obstetricians in situations where "evidence" is weak or lacking. Answers with a recommendation level of A or B represent current standard care practices in Japan. All 113 CQAs and the appendix are presented here to promote a better understanding of the current standard care practices for pregnant and lactating women in Japan.

Published
2022
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26. Chemical enrichment in the Centaurus cluster of galaxies

Author

Fukushima, Kotaro, Kobayashi, Shogo B., and Matsushita, Kyoko

Subjects
X-ray astronomy, XMM-Newton, intracluster medium
Abstract

Contributed talk in "Exploring the Hot and Energetic Universe: the 3rd scientific conference dedicated to the Athena X-ray Observatory". This presentation is based on the published paper "Chemical enrichment in the cool core of the Centaurus cluster of galaxies" (Fukushima et al., 2022, MNRAS, 514, 4222)., This work is financially supported by the Japanese Society for the Promotion of Science (JSPS) through the Grant-in-Aid for JSPS Fellows grant No. 21J21541 (KF).

Published
2022
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34. Feasibility of a mobile cardiotocogram device for fetal heart rate self‐monitoring in low‐risk singleton pregnant women

Author

Tamaru, Shunsuke, primary, Jwa, Seung Chik, additional, Ono, Yoshihisa, additional, Seki, Hiroyuki, additional, Matsui, Haruka, additional, Fujii, Tatsuya, additional, Iriyama, Takayuki, additional, Doi, Koutarou, additional, Sameshima, Hiroshi, additional, Naruse, Katsuhiko, additional, Kobayashi, Hiroshi, additional, Yoshida, Rie, additional, Nishi, Hirotaka, additional, Hirata, Yoshiyasu, additional, Fukushima, Kotaro, additional, Hirakawa, Toshio, additional, Nakano, Yoshihiro, additional, Asakawa, Yasuyuki, additional, Tsunoda, Yutaka, additional, Oda, Toshimitsu, additional, Nii, Shigeru, additional, Fujii, Tomoyuki, additional, Kinoshita, Katsuyuki, additional, and Kamei, Yoshimasa, additional

Published
2021
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39. soft X-ray background with Suzaku. I. Milky Way halo.

Author

Ueda, Masaki, Sugiyama, Hayato, Kobayashi, Shogo B, Fukushima, Kotaro, Yamasaki, Noriko Y, Sato, Kosuke, and Matsushita, Kyoko

Subjects
MILKY Way, GALACTIC center, CHARGE exchange, HYDROSTATIC equilibrium, SOLAR cycle, SOFT X rays
Abstract

We present measurements of the soft X-ray background emission for 130 Suzaku observations at 75° < l < 285° and | b | > 15° obtained from 2005 to 2015, covering nearly one solar cycle. In addition to the standard soft X-ray background model consisting of the local hot bubble and the Milky Way Halo (MWH), we include a hot collisional-ionization-equilibrium component with a temperature of ∼0.8 keV to reproduce spectra of a significant fraction of the lines of sight. Then, the scatter in the relation between the emission measure vs. temperature of the MWH component is reduced. Here, we exclude time ranges with high count rates to minimize the effect of the solar wind charge exchange (SWCX). However, the spectra of almost the same lines of sight are inconsistent. The heliospheric SWCX emissions likely contaminate and give a bias in measurements of temperature and the emission measure of the MWH. Excluding the data around the solar maximum and using the data taken before the end of 2009, at | b | > 35° and 105° < l < 255°, the temperature (0.22 keV) and emission measure (2 × 10−3 cm−6 pc) of the MWH are fairly uniform. The increase of the emission measure toward the lower Galactic latitude at | b | < 35° indicates the presence of a disk-like morphology component. A composite model which consists of disk-like and spherical-morphology components also reproduces the observed emission measure distribution of MWH. In this case, the hydrostatic mass at a few tens of kiloparsec from the Galactic center agrees with the gravitational mass of the Milky Way. The plasma with the virial temperature likely fills the Milky Way halo in nearly hydrostatic equilibrium. Assuming a gas metallicity of 0.3 solar, the upper limit of the gas mass of the spherical component out to 250 kpc, or the virial radius, is ∼ a few × 1010  M ⊙. [ABSTRACT FROM AUTHOR]

Published
2022
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