原子分子応用-ezoe.key
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- さみ くだら
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3 X kev (kev-tev), ( ~1000 ),,, X ( ) ( ) 80% X ~100 (Fukugita & Peebles 2004, Read & Trentham 2005 )
4 日本のX線天文衛星 宇宙からのX線は地球大気で吸収, 飛翔体が不可欠 日本は継続した衛星計画で世界を牽引, 活動的宇宙を明らかに XMM-Newton EXOSAT ROSAT X Beppo-SAX Granat Ufuru Einstein Chandra RXTE Japan 417 kg 420 kg Hakucho ASCA Ginga 2015 NuSTAR 1680 kg 216 kg 96 kg Swift ASTRO-H 2700 kg 2020 (Year) Suzaku Tenma
5 14 m, 2700 kg Low earth orbit 550 km, 31 CCD 1. High Resolution Spectroscopy by a micro-calorimeter array X-ray Telescopes Si/CdTe Compton Camera Extended objects, Fe K lines 2. Wide-Band/High Sensitivity Observation kev, thermal + nonthermal emissions Micro Calorimeter Si/CdTe Imager
6 The ASTRO-H X-ray Observatory Tadayuki Takahashi a, Kazuhisa Mitsuda a, Richard Kelley b,henriaarts c, Felix Aharonian d, Hiroki Akamatsu c, Fumie Akimoto e, Steve Allen f, Naohisa Anabuki g, Lorella Angelini b, Keith Arnaud h,makotoasai f,marcaudard i, Hisamitsu Awaki j, Philipp Azzarello i, Chris Baluta a,ayabamba k,nobutakabando a,markbautz l, Roger Blandford f, Kevin Boyce b,gregbrown m,edcackett n, Maria Chernyakova d, Paolo Coppi o, Elisa Costantini c, Jelle de Plaa c, Jan-Willem den Herder c, Michael DiPirro b, Chris Done p,tadayasudotani a,johndoty q, Ken Ebisawa a,meganeckart b, Teruaki Enoto r, Yuichiro Ezoe s, Andrew Fabian n, Carlo Ferrigno i,adamfoster t, Ryuichi Fujimoto u,yasushifukazawa v,stefanfunk f, Akihiro Furuzawa e, Massimiliano Galeazzi w, Luigi Gallo x,poshakgandhi a, Keith Gendreau b, Kirk Gilmore f, Daniel Haas c, Yoshito Haba e,kenjihamaguchi h,isamuhatsukade y,takayukihayashi a, Kiyoshi Hayashida g, Junko Hiraga z, Kazuyuki Hirose a, Ann Hornschemeier b, Akio Hoshino u,johnhughes aa,unahwang ab, Ryo Iizuka ac, Yoshiyuki Inoue f, Kazunori Ishibashi e, Manabu Ishida a, Kosei Ishimura a, Yoshitaka Ishisaki s,masayukiito ad, Naoko Iwata a,naokoiyomoto ae, Jelle Kaastra c, Timothy Kallman b,tuneyoshikamae f, Jun Kataoka af,satorukatsuda r, Hajime Kawahara s,madokakawaharada a, Nobuyuki Kawai ag, Shigeo Kawasaki a, Dmitry Khangaluyan a, Caroline Kilbourne b, Masashi Kimura g, Kenzo Kinugasa ah, Shunji Kitamoto ai, Tetsu Kitayama aj, Takayoshi Kohmura ak, Motohide Kokubun a,tatsurokosaka al, Alex Koujelev am, Katsuji Koyama an, Hans Krimm b,ayakubota ao, Hideyo Kunieda e, Stephanie LaMassa o, Philippe Laurent ap, François Lebrun ap, Maurice Leutenegger b, Olivier Limousin ap, Michael Loewenstein b,knoxlong aq, David Lumb ar,grzegorzmadejski f, Yoshitomo Maeda a, Kazuo Makishima z,genevièvemarchand am, Maxim Markevitch b, Hironori Matsumoto e, Kyoko Matsushita as,danmccammon at, Brian McNamara au, Jon Miller av, Eric Miller l, Shin Mineshige an, Kenji Minesugi a, Ikuyuki Mitsuishi s, Takuya Miyazawa e, Tsunefumi Mizuno v, Hideyuki Mori a,kojimori y,kojimukai b, Toshio Murakami u, Hiroshi Murakami ai, Richard Mushotzky h,houseinagano e, Ryo Nagino g,takaonakagawa a, Hiroshi Nakajima g,takeshinakamori af, Kazuhiro Nakazawa z, Yoshiharu Namba aw, Chikara Natsukari a, Yusuke Nishioka y, Masayoshi Nobukawa an,masaharunomachi g, Steve O Dell ax, Hirokazu Odaka a, Hiroyuki Ogawa a, Mina Ogawa a, Keiji Ogi j,takayaohashi s,masanoriohno v, Masayuki Ohta a, Takashi Okajima b,atsushiokamoto ay,tsuyoshiokazaki a,naomiota az, Masanobu Ozaki a, Frits Paerels ba, Stéphane Paltani i, Arvind Parmar bb,robertpetre b, Martin Pohl i, F.Scott Porter b, Brian Ramsey ax, Rubens Reis av, Christopher Reynolds h, Helen Russell au,samarsafi-harb bc, Shin-ichiro Sakai a, Hiroaki Sameshima a, Jeremy Sanders n,gorosato a, Rie Sato a, Yoichi Sato ay,kosukesato as,makotosawada k, Peter Serlemitsos b, Hiromi Seta ai, Yasuko Shibano a, Maki Shida a, Takanobu Shimada a, Keisuke Shinozaki ay, Peter Shirron b, Aurora Simionescu f, Cynthia Simmons b, Randall Smith t, Gary Sneiderman b,yangsoong b,lukaszstawarz a,yasuharusugawara ac, Hiroyuki Sugita ay, Satoshi Sugita e, Andrew Szymkowiak o, Hiroyasu Tajima e, Hiromitsu Takahashi v, Shin-ichiro Takeda a,yohtakei a,torutamagawa r, Takayuki Tamura a, Keisuke Tamura e,takaakitanaka an,yasuotanaka a, Makoto Tashiro bd,yuzurutawara e, Yukikatsu Terada bd, Yuichi Terashima j, Francesco Tombesi b, Hiroshi Tomida a,yokotsuboi ac, Masahiro Tsujimoto a, Hiroshi Tsunemi g,takeshitsuru an, Hiroyuki Uchida an, Yasunobu Uchiyama f, Hideki Uchiyama z, Yoshihiro Ueda an, Shiro Ueno ay, Shinichiro Uno be,megurry o, Eugenio Ursino w, Cor de Vries c,atsushiwada ay, Shin Watanabe a,norbertwerner f, Nicholas White b, Takahiro Yamada a, Shinya Yamada r, Hiroya Yamaguchi t, Noriko Yamasaki a, Shigeo Yamauchi az,makotoyamauchi y, Yoichi Yatsu ag, Daisuke Yonetoku u, Atsumasa Yoshida k Takayuki Yuasa a Takahashi+12 SPIE Science March
7 PI : JAXA
8 @ kev ΔE (FWHM) <7 5.9 kev (CCD 20 ) >2 kev E X X E~1 fj ΔT = E/C ~ 1 mk C ~ 1pJ/K 6x6 (5 mm = 3 ) µm HgTe - Si 50 mk 0.95 m kg W - X
9 X electron hole pair ASTRO-H SXI - 4 CCD chips - 62 mm = 38 ΔE (FWHM) ~ kev Mega pixel = imager X ΔE (FWHM) ~1 1 kev, ~ kev ΔE X
10 good Resolving Power (E/ΔE) ( ) HEG MEG LETG RGS He-like triplet, ASTRO-H SXS 4 ev ( ) 7 ev ( ) doppler shift (100 km/s, 100 photon) X CCD H-He like ion K X (kev)
11 1000 good ASTRO-H SXS SXS Effective Area (cm 2 ) (cm 2 ) 100 RGS MEG HEG 10 LETG Energy (kev) X (kev) 10
12 55Fe (Mn Kα) Kα2 55Fe (Mn Kα) pixel Kα1 FWHM 4.53 ev! * * Baseline = signal baseline
13 3 (X, Chandra) Counts s -1 kev -1 Fe CCD Response Z = (3420 km/sec) Fe-L Ne Mg O S Si S (Fe K ) ASTRO-H SXS simulation Ar Ca Fe Mitsuda+10
14 Perseus (Chandra) total energy = : (, ) 1' = 22 kpc bulk motion (line shift)? (line broadening)? ASTRO-H White paper
15 ,? : Fe K (Mpc -3 ) z ( ) Ueda+07
16 , large n, n target (, ), ( ), CX simulation e.g., O 7+ + H O 6+ + H + + hν Dennerl+04 Gladstone+02 Ezoe+13
17 He 1. He = Porous Plug (PP) 2. film flow <2 µg/s = knife edge device, He PP PP He PP edge stop Φ8.9 mm, t6.3 mm Si chip, 10 mm ( ) Si (110) plane Ishikawa+10 Ezoe+15 He tank Si (111) plane 50 nm 10 nm
18 DIOS : beyond ASTRO-H W 吸収体無 再評価 9 kev達成!! 動作点5000 mvでのノイズスペクトル PI 大橋 : ASTRO-H の次を狙う, 広視野X線カロリメータミッション 量が小さく e を分解でき はないか り上がりが 16x16 pixel, <5 ev 0.6 kev, 50分角 Yoshikawa+01 SΩ=100 cm2 deg2, ASTRO-H の~100倍 2008 データ長 10k バンド幅 500 khz 2009 データ長 100k バンド幅 40 khz baryon の探査 (全バリオンの ~20-30 %) missing 3 cm 暗黒物質 銀河 missing baryon K 銀河団 K 1 cm Ezoe+09, 15 数 log R 衛星外観図 -軌道上コンフィグレーション- α 常伝導状態 Z Baseline 分解能 遷移端 カロリメータグループミーティング 超伝導状態 幅 数 mk MnKα 分解能 補正済み 4 超伝導薄膜温度計 Y 12&m X線カロリアレイ log T X 2022年頃を目指し提案予定 重量 690 kg, 電力 700 W 図 5: DIOS 衛星の外観図 2014 年度の検討でバスと観測系を一体設計とし 従来デザインよりコンパクト
19 X & SDD X & DepFET X ~10 g, 1-3 Ezoe+10 X
20 , Fe K, :,, DIOS, X ORBIS, GEO-X pathfinder,
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21 1 1 1 2 2 5 7 9 11 13 13 14 18 18 20 28 28 29 31 31 34 35 35 36 37 37 38 39 40 56 66 74 89 99 - ------ ------ -------------- ---------------- 1 10 2-2 8 5 26 ( ) 15 3 4 19 62 2,000 26 26 5 3 30 1 13
The ASTRO-H (Hitomi) x-ray astronomy satellite The MIT Faculty has made this article openly available. Please share how this access benefits you. Your
The ASTRO-H (Hitomi) x-ray astronomy satellite The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation As Published Publisher Takahashi,
The ASTRO-H (Hitomi) x-ray astronomy satellite The MIT Faculty has made this article openly available. Please share how this access benefits you. Your
The ASTRO-H (Hitomi) x-ray astronomy satellite The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation As Published Publisher Takahashi,
Atmospheric gas dynamics in the Perseus cluster observed with Hitomi
Atmospheric gas dynamics in the Perseus cluster observed with Hitomi Hitomi collaboration Shutaro Ueda, Yuto Ichinohe Ryuichi Fujimoto, Shota Inoue, Caroline Kilbourne, Tetsu Kitayama, Maxim Markevitch,
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1/8 A. 電気所 ( 発電所, 変電所, 配電塔 ) における変圧器の空き容量一覧 < 留意事項 > (1) 空容量は目安であり 系統接続の前には 接続検討のお申込みによる詳細検討が必要となります その結果 空容量が変更となる場合があります (2) 特に記載のない限り 熱容量を考慮した空き容量を記載しております その他の要因 ( や系統安定度など ) で連系制約が発生する場合があります (3)
空き容量一覧表（154kV以上）
1/3 A. 電気所 ( 発電所, 変電所, 配電塔 ) における変圧器の空き容量 覧 < 留意事項 > (1) 空容量は 安であり 系統接続の前には 接続検討のお申込みによる詳細検討が必要となります その結果 空容量が変更となる場合があります (2) 熱容量を考慮した空き容量を記載しております その他の要因 ( や系統安定度など ) で連系制約が発 する場合があります (3) 表 は 既に空容量がないため
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(a) (b) (c) (d) (e) (f) (g) (f) (a), (b) 1 He Gleiter 1) 5-25 nm 1/2 Hall-Petch 10 nm Hall-Petch 2) 3) 4) 2 mm 5000% 5) 1(e) 20 µm Pd, Zr 1(f) Fe 6) 10 nm 2 8) Al-- 1,500 MPa 9) 2 Fe 73.5 Si 13.5 B 9 Nb
1/68 A. 電気所 ( 発電所, 変電所, 配電塔 ) における変圧器の空き容量一覧 平成 31 年 3 月 6 日現在 < 留意事項 > (1) 空容量は目安であり 系統接続の前には 接続検討のお申込みによる詳細検討が必要となります その結果 空容量が変更となる場合があります (2) 特に記載
1/68 A. 電気所 ( 発電所, 変電所, 配電塔 ) における変圧器の空き容量一覧 平成 31 年 3 月 6 日現在 < 留意事項 > (1) 空容量は目安であり 系統接続の前には 接続検討のお申込みによる詳細検討が必要となります その結果 空容量が変更となる場合があります (2) 特に記載のない限り 熱容量を考慮した空き容量を記載しております その他の要因 ( 電圧や系統安定度など ) で連系制約が発生する場合があります
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X線分析の進歩36 別刷
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