研究者業績

片坐 宏一

カタザ ヒロカズ  (Hirokazu KATAZA)

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

J-GLOBAL ID
202001007925227103
researchmap会員ID
R000009969

論文

 200
  • Hirokazu Kataza, Ryouhei Kano, Naoteru Gouda, Masayuki Hirabayashi, Naoki Isobe, Takafumi Kamizuka, Shingo Kashima, Hajime Kawahara, Daisuke Kawata, Naoki Kohara, Iona Kondo, Ichiro Mase, Kohei Miyakawa, Ryou Ohsawa, Masanobu Ozaki, Risa Shimizu, Yoshinori Suematsu, Shotaro Tada, Toshihiro Tsuzuki, Fumihiro Uraguchi, Fumihiko Usui, Shin Utsunomiya, Takehiko Wada, Yoshiyuki Yamada, Taihei Yano
    Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave 9-9 2024年8月23日  
  • Takafumi Kamizuka, Hajime Kawahara, Ryou Ohsawa, Hirokazu Kataza, Daisuke Kawata, Yoshiyuki Yamada, Teruyuki Hirano, Kohei Miyakawa, Masataka Aizawa, Masashi Omiya, Taihei Yano, Ryouhei Kano, Takehiko Wada, Wolfgang Loeffler, Michael Biermann, Pau Ramos, Naoki Isobe, Fumihiko Usui, Kohei Hattori, Satoshi Yoshikawa, Takayuki Tatekawa, Hideyuki Izumiura, Akihiko Fukui, Makoto Miyoshi, Daisuke Tatsumi, Naoteru Gouda
    Modeling, Systems Engineering, and Project Management for Astronomy XI 93-93 2024年8月23日  
  • Naoki Isobe, Shingo Kashima, Yoshinori Suematsu, Naoteru Gouda, Ryohei Kano, Hirokazu Kataza, Hajime Kawahara, Naoki Kohara, Iona Kondo, Ichiro Mase, Ryou Ohsawa, Toshihiro Tsuzuki, Fumihiko Usui, Shin Utsunomiya, Takehiko Wada, Yoshiyuki Yamada, Taihei Yano, Aoi Takahashi, Tomoya Hattori, Koichi Takeda, Yukina Arima
    Proceedings of SPIE - The International Society for Optical Engineering 13092 2024年  
    Structural, Thermal and Optical Performance (STOP) analysis is performed to investigate the stability of the telescope to be onboard the Japan Astrometry Satellite Mission for INfrared Exploration (JASMINE). In order to perform one of the prime science objectives, high-precision astrometric observations in the wavelength range of 1.0–1.6 µm toward the Galactic center to reveal its central core structure and formation history, the JASMINE telescope is requested to be highly stable with an orbital change in the image distortion pattern being less than a few 10 µas after low-order correction. The JASMINE telescope tried to satisfy this requirement by adopting two design concepts. Firstly, the mirror and their support structures are made of extremely low coefficient-of-thermal-expansion materials. Secondly, their temperatures are highly stabilized with an orbital variation of less the 0.1 ◦C by the unique thermal control idea. Through the preliminary STOP analysis, the structural and thermal structural feasibility of the JASMINE telescope is considered. By combining the results of the structural and thermal design, its thermal deformation is estimated. The optical performance of the JASMINE telescope after the thermal deformation is numerically evaluated. It is found that the thermal displacement of the mirrors in the current structural thermal design produces a slightly large focus-length change. As far as the focus adjustment is adequately applied, the orbital variation of the image distortion pattern is suggested to become acceptable after the low-order correction.
  • Takafumi Kamizuka, Takashi Miyata, Shigeyuki Sako, Ryou Ohsawa, Kentaro Asano, Atsushi Nishimura, Kengo Tachibana, Tsubasa Michifuji, Hirokazu Iida, Akira C. Naruse, Mizuho Uchiyama, Itsuki Sakon, Takashi Onaka, Hirokazu Kataza, Sunao Hasegawa, Fumihiko Usui, Naruhisa Takato, Noboru Ebizuka, Takuya Hosobata, Tsutomu Aoki, Mamoru Doi, Fumi Egusa, Bunyo Hatsukade, Natsuko Kato, Kotaro Kohno, Masahiro Konishi, Shintaro Koshida, Shuhei Koyama, Takeo Minezaki, Tomoki Morokuma, Kentaro Motohara, Mizuki Numata, Hiroaki Sameshima, Hidenori Takahashi, Yoichi Tamura, Toshihiko Tanabe, Masuo Tanaka, Kosuke Kushibiki, Nuo Chen, Shogo Homan, Yuzuru Yoshii
    Proceedings of SPIE, Ground-based and Airborne Instrumentation for Astronomy IX 12184 2022年8月29日  
    MIMIZUKU is the first-generation mid-infrared instrument for the TAO 6.5-m telescope. It has three internal optical channels to cover a wide wavelength range from 2 to 38 mu m. Of the three channels, the NIR channel is responsible for observations in the shortest wavelength range, shorter than 5.3 mu m. The performance of the NIR channel is evaluated in the laboratory. Through the tests, we confirm the followings: 1) the detector (HAWAII-1RG with 5.3-mu m cutoff) likely achieves similar to 80% quantum efficiency; 2) imaging performance is sufficient to achieve seeing-limit spatial resolution; 3) system efficiencies in imaging modes are 2.4-31%; and 4) the system efficiencies in spectroscopic modes is 5-18%. These results suggest that the optical performance of the NIR channel is achieved as expected from characteristics of the optical components. However, calculations of the background levels and on-sky sensitivity based on these results suggest that neutral density (ND) filters are needed to avoid saturation in L'- and M'-band observations and that the ND filters and the entrance window, made of chemical-vapor-deposition (CVD) diamond, significantly degrade the sensitivity in these bands. This means that the use of different window materials and improvements of the detector readout speed are required to achieve both near-infrared and long-wavelength mid-infrared (>30 mu m) observations.
  • Kunimoto Komatsu, Hirokazu Ishino, Hirokazu Kataza, Kuniaki Konishi, Makoto Kuwata-Gonokami, Nobuhiko Katayama, Shinya Sugiyama, Tomotake Matsumura, Haruyuki Sakurai, Yuki Sakurai, Ryota Takaku, Junji Yumoto
    Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X 11453 2020年12月18日  
    We have developed a prototype half-wave plate (HWP) based polarization modulator (PMU) for Cosmic Microwave Background polarization measurement experiments. We built a 1/10 scaled PMU that consists of a 50 mm diameter five-layer achromatic HWP with a moth-eye broadband anti-reflection sub-wavelength structure mounted on a superconducting magnetic bearing. The entire system has cooled below 20 K in a cryostat chamber that has two millimeter-wave transparent windows. A coherent source and the diode detector are placed outside of the cryostat and the millimeter-wave goes through the PMU in the cryostat. We have measured the modulated signal by the PMU, analyzed the spectral signatures, and extracted the modulation efficiency over the frequency coverage of 34-161 GHz. We identified the peaks in the optical data, which are synchronous to the rotational frequency. We also identified the peaks that are originated from the resonance frequency of the levitating system. We also recovered the modulation efficiency as a function of the incident electromagnetic frequency and the data agrees to the predicted curves within uncertainties of the input parameters, i.e.The indices of refraction, thickness, and angle alignment. Finally, we discuss the implication of the results when this is applied to the LiteBIRD low-frequency telescope.

MISC

 155
  • 郷田直輝, 鹿野良平, 辻本拓司, 矢野太平, 上田暁俊, 三好真, 辰巳大輔, 馬場淳一, 鹿島伸悟, 小宮山裕, 片坐宏一, 臼井文彦, 山田良透, 河田大介, 西亮一, 河原創
    日本天文学会年会講演予稿集 2021 2021年  
  • 山田良透, LOEFFLER Wolfgang, 郷田直輝, 矢野太平, 辰巳大輔, 片坐宏一, 吉岡諭
    日本天文学会年会講演予稿集 2021 2021年  
  • 片坐宏一, 臼井文彦, 山田良透, 郷田直輝, 鹿野良平, 矢野太平, 上田暁俊, 三好真, 辰巳大輔, 鹿島伸悟, 小宮山裕
    日本天文学会年会講演予稿集 2021 2021年  
  • 矢野太平, 郷田直輝, 三好真, 上田暁俊, 辰巳大輔, 鹿島伸悟, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2021 2021年  
  • 鹿野良平, 郷田直輝, 上田暁俊, 小宮山裕, 満田和久, 中屋秀彦, 片坐宏一, 臼井文彦, 山田良透
    日本天文学会年会講演予稿集 2021 2021年  
  • 鹿島伸悟, 矢野太平, 上田暁俊, 辰巳大輔, 小宮山裕, 鹿野良平, 郷田直輝, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2021 2021年  
  • 矢野太平, 郷田直輝, 鹿野良平, 三好真, 上田暁俊, 辰巳大輔, 鹿島伸悟, 山田良透, 片坐宏一, 臼井文彦
    日本天文学会年会講演予稿集 2021 2021年  
  • 郷田直輝, 鹿野良平, 辻本拓司, 矢野太平, 上田暁俊, 三好真, 辰巳大輔, 馬場淳一, 鹿島伸悟, 小宮山裕, 末松芳法, 片坐宏一, 臼井文彦, 磯部直樹, 内山瑞穂, 山田良透, 河田大介, 西亮一, 河原創
    日本天文学会年会講演予稿集 2021 2021年  
  • 大宮正士, 大宮正士, 山田良透, 河田大介, 上塚貴史, 河原創, 大澤亮, 片坐宏一, 立川崇之, 服部公平, 平野照幸, 平野照幸, 福井暁彦, 吉岡諭, LOEFFLER Wolfgang, 臼井文彦, 泉浦秀行, 三好真, 矢野太平, 辰巳大輔, 郷田直輝
    日本天文学会年会講演予稿集 2021 2021年  
  • 矢野太平, 郷田直輝, 上田暁俊, 辰巳大輔, 三好真, 鹿島伸悟, 間瀬一郎, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2020 2020年  
  • 郷田直輝, 辻本拓司, 矢野太平, 上田暁俊, 三好真, 辰巳大輔, 馬場淳一, 鹿島伸悟, 間瀬一郎, 山田良透, 河田大介, 片坐宏一, 西亮一, 吉岡諭, 河原創
    日本天文学会年会講演予稿集 2020 2020年  
  • 山田良透, LOEFFLER Wolfgang, 郷田直輝, 矢野太平, 辰巳大輔, 片坐宏一, 吉岡諭, 穂積俊輔
    日本天文学会年会講演予稿集 2020 2020年  
  • 鹿島伸悟, 矢野太平, 上田暁俊, 辰巳大輔, 三好真, 井上登志夫, 宇都宮真, 間瀬一郎, 郷田直輝, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2020 2020年  
  • 上田暁俊, 間瀬一郎, 辰巳大輔, 宇都宮真, 鹿島伸悟, 矢野太平, 郷田直輝, 三好真, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2020 2020年  
  • 矢野太平, 郷田直輝, 上田暁俊, 辰巳大輔, 三好真, 鹿島伸悟, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2020 2020年  
  • 上田暁俊, 間瀬一郎, 辰巳大輔, 宇都宮真, 鹿島伸悟, 矢野太平, 郷田直輝, 三好真, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2020 2020年  
  • 郷田直輝, 辻本拓司, 矢野太平, 上田暁俊, 三好真, 辰巳大輔, 馬場淳一, 鹿島伸悟, 山田良透, 河田大介, 片坐宏一, 片坐宏一, 西亮一, 河原創
    日本天文学会年会講演予稿集 2020 2020年  
  • 山田良透, LOEFFLER Wolfgang, 郷田直輝, 矢野太平, 辰巳大輔, 片坐宏一, 吉岡諭
    日本天文学会年会講演予稿集 2020 2020年  
  • 鹿島伸悟, 矢野太平, 上田暁俊, 辰巳大輔, 三好真, 井上登志夫, 宇都宮真, 間瀬一郎, 郷田直輝, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2019 2019年  
  • 山田良透, LOEFFLER Wolfgang, 郷田直輝, 矢野太平, 辰巳大輔, 片坐宏一, 吉岡諭, 穂積俊輔
    日本天文学会年会講演予稿集 2019 2019年  
  • 中川貴雄, 小川博之, 篠崎慶亮, 竹内伸介, 大坪貴文, 片坐宏一, 後藤健, 西城大, 佐藤洋一, 澤田健一郎, 東谷千比呂, 長勢晃一, 松原英雄, 松本純, 水谷忠均, 山田亨, 山村一誠, 金田英宏, 芝井広
    日本天文学会年会講演予稿集 2019 2019年  
  • 上田暁俊, 間瀬一郎, 辰巳大輔, 井上登志夫, 宇都宮真, 鹿島伸悟, 矢野太平, 郷田直輝, 三好真, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2019 2019年  
  • 矢野太平, 郷田直輝, 上田暁俊, 辰巳大輔, 三好真, 鹿島伸悟, 間瀬一郎, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2019 2019年  
  • 郷田直輝, 辻本拓司, 矢野太平, 上田暁俊, 三好真, 辰巳大輔, 馬場淳一, 鹿島伸悟, 間瀬一郎, 山田良透, 河田大介, 片坐宏一, 西亮一, 河原創
    日本天文学会年会講演予稿集 2019 2019年  
  • 矢野太平, 郷田直輝, 上田暁俊, 三好真, 辰巳大輔, 宇都宮真, 鹿島伸悟, 間瀬一郎, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2019 2019年  
  • 上田暁俊, 間瀬一郎, 宇都宮真, 鹿島伸悟, 矢野太平, 郷田直輝, 井上登志夫, 辰巳大輔, 三好真, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2019 2019年  
  • 鹿島伸悟, 矢野太平, 上田暁俊, 辰巳大輔, 三好真, 井上登志夫, 宇都宮真, 間瀬一郎, 郷田直輝, 山田良透, 片坐宏一
    日本天文学会年会講演予稿集 2019 2019年  
  • 郷田直輝, 辻本拓司, 矢野太平, 上田暁俊, 三好真, 辰巳大輔, 馬場淳一, 宇都宮真, 鹿島伸悟, 間瀬一郎, 亀谷收, 浅利一善, 山田良透, 河田大介, 片坐宏一, 西亮一, 中須賀真一
    日本天文学会年会講演予稿集 2019 2019年  
  • 中村 友彦, 宮田 隆志, 酒向 重行, 上塚 貴史, 浅野 勝晃, 内山 瑞穂, 尾中 敬, 板 由房, 米田 瑞生, 片坐 宏一, Nakamura Tomohiko, Miyata Takashi, Sako Shigeyuki, Kamizuka Takafumi, Asano Katsuaki, Uchiyama Mizuho, Onaka Takashi, Ita Yoshifusa, Yoneda Mizuki, Kataza Hirokazu
    宇宙航空研究開発機構特別資料 = JAXA Special Publication: Proceedings of the SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (17) 249-251 2018年3月9日  
    著者人数: 29名形態: カラー図版あり資料番号: AA1730027053レポート番号: JAXA-SP-17-010E
  • 下村俊貴, 寺地祐介, 寺尾悠, 大崎博之, 桜井雄基, 松村知岳, 片山伸彦, 菅井肇, 今田大皓, 山本亮, 宇都宮真, 片坐宏一
    電磁力関連のダイナミクスシンポジウム講演論文集 29th 2017年  
  • 桜井雄基, 松村知岳, 飯田光人, 片山伸彦, 菅井肇, 大崎博之, 寺尾悠, 寺地祐介, 下村俊貴, 今田大皓, 山本亮, 宇都宮真, 片坐宏一
    電磁力関連のダイナミクスシンポジウム講演論文集 29th 2017年  
  • 下村俊貴, 寺地祐介, 寺尾悠, 大崎博之, 桜井雄基, 松村知岳, 片山伸彦, 菅井肇, 今田大皓, 山本亮, 宇都宮真, 片坐宏一
    低温工学・超電導学会講演概要集 94th 2017年  
  • 松村知岳, 桜井雄基, 片山伸彦, 菅井肇, 下村俊貴, 寺地祐介, 寺尾悠, 大崎博之, 今田大皓, 山本亮, 宇都宮真, 片坐宏一
    低温工学・超電導学会講演概要集 94th 2017年  
  • 寺地祐介, 寺尾悠, 大崎博之, 桜井雄基, 松村知岳, 菅井肇, 宇都宮真, 片坐宏一, 山本亮
    MAGDAコンファレンス講演論文集 25th 2016年  
  • 片坐宏一, 岡本美子, 本田充彦, 左近樹
    日本天文学会年会講演予稿集 2015 2015年  
  • 片坐宏一, 村田泰宏, 浅野健太朗
    日本天文学会年会講演予稿集 2015 2015年  
  • 本田 充彦, Maaskant Koen, 岡本 美子, 岡本 美子, Okamoto Yoshiko K., 片坐 宏一, Kataza Hirokazu, 山下 卓也, Yamashita Takuya, 宮田 隆志, Miyata Takashi, 酒向 重行, Sako Shigeyuki, 藤吉 拓哉, Fujiyoshi Takuya, 左近 樹, Sakon Itsuki, 藤原 英明, Fujiwara Hideaki, 上塚 貴史, Kamizuka Takafumi, Mulders Gijs D., Lopez-Rodriguez Enrique, Packham Christpher, 井上 昭雄, Inoue Akio K., 尾中 敬, Onaka Takashi
    Science journal of Kanagawa University 26 23-31 2015年  
    We imaged circumstellar disks around 22 Herbig Ae/Be stars at 25 μm using Subaru/COMICS and Gemini/T-ReCS. Our sample consisted of 11 group I (flaring disk) andgroup II (flat disk) sources. We found that group I sources tended to show more extended emission than group II sources. Previous studies showed that the continuous disk is hard to resolve with 8-meter-class telescopes in the Q-band due to the strong emissions from the unresolved innermost region of the disk. This indicates that Q-band resolution sources requires a hole orgap in the disk material distribution to suppress the contribution from the innermost region of the disk. As many group I sources are resolved at 25 μm, we suggest that many, not all, group I Herbig Ae/Be disks have a hole or gap and are (pre-)transitional disks. On the other hand, the unresolved nature of many group II sources at 25 μm supports the suggestion that group II disks have a continuous, flat disk geometry. It has been inferred that group I disks may evolve into group II through the settling of dust grains at the mid-plane of the proto-planetary disk. However, considering growing evidence of the presence of a hole or gaps in the disk of group I sources, such an evolutionary scenario is unlikely. The difference between groups I and II may reflect different evolutionary pathways of protoplanetary disks..原著2014 年度神奈川大学総合理学研究所共同研究助成論文
  • 片坐宏一, 和田武彦, 猿楽祐樹, 左近樹, 小林尚人
    日本天文学会年会講演予稿集 2014 2014年  
  • 左近樹, 尾中敬, 片坐宏一, 岡本美子, 本田充彦, 所仁志, 藤代尚文, 藤代尚文, 池田優二, 中川寛之, 桐野宙治, 三ツ井健司, 岡田則夫
    日本天文学会年会講演予稿集 2014 2014年  
  • 左近樹, 尾中敬, 本田充彦, 片坐宏一, 岡本美子, 所仁志, 藤代尚文, 藤代尚文, 池田優二, 中川寛之, 桐野宙治, 三ツ井健司, 岡田則夫
    日本天文学会年会講演予稿集 2014 2014年  
  • 片坐宏一, 和田武彦, 猿楽祐樹, 左近樹, 小林尚人, 大藪進喜
    日本天文学会年会講演予稿集 2013 2013年  
  • 左近樹, KEMPER Francisa, 片坐宏一, 和田武彦, 猿楽祐樹, 下西隆, 大藪進喜, 尾中敬, 大山陽一, 松本敏雄, 高見道弘, FOUCAUD Sebastien, ZHAO-GEISLER Ronny, SRINIVASAN Sundar, WU Ronin
    日本天文学会年会講演予稿集 2013 2013年  
  • 片坐宏一, 和田武彦, 猿楽祐樹, 左近樹, 小林尚人, 大藪進喜
    日本天文学会年会講演予稿集 2012 2012年  
  • 和田武彦, 片坐宏一
    日本天文学会年会講演予稿集 2012 2012年  
  • 片坐宏一, 和田武彦, 猿楽祐樹, 左近樹, 小林尚人, 大藪進喜
    日本天文学会年会講演予稿集 2012 2012年  
  • 本田 充彦, Maaskant Koen, 岡本 美子, Okamoto Yoshiko K., 片坐 宏一, Kataza Hirokazu, 深川 美里, Fukagawa Misato, Waters Lawrens B. F. M., Dominik Carsten, Tielens Alexander G. G. M., Mulders Gijs D., Michel Min, 山下 卓也, Yamashita Takuya, 藤吉 拓哉, Fujiyoshi Takuya, 宮田 隆志, Miyata Takashi, 酒向 重行, Sako Shigeyuki, 左近 樹, Sakon Itsuki, 藤原 英明, Fujiwara Hideaki, 尾中 敬, Onaka Takashi, Koen Maaskant
    Science journal of Kanagawa University 23 1-10 2012年  
    The disk around the Herbig Ae star HD169142 was imaged and resolved at 18.8 and 24.5 μm using Subaru/COMICS. We interpreted the observations using a 2D radiative transfer model and found evidence for the presence of a large gap.MIR images trace dust emits at the onset of a strong rise in the spectral energy distribution(SED)at 20 μm;therefore,they are very sensitive to the location and characteristics of the inner wall of the outer disk and its dust.We determined the location of the wall to be 23 +3 -5 AU from the star.An extra component of hot dust must therefore exist close to the star.We found that a hydrostatic optically thick inner disk does not produce enough flux in the NIR and an optically thin geometrically thick component was our solution to fit the SED.Considering the recent findings of gaps and holes in a number of Herbig Ae/Be group I disks,we suggest that such disk structures may be common in group I sources.Classification as group I should be considered to support the classification as a transitional disk,although improved imaging surveys are needed to support this speculation.原著 2011 年度神奈川大学総合理学研究所共同研究助成論文
  • 片坐宏一, 和田武彦, 左近樹, 小林尚人
    日本天文学会年会講演予稿集 2011 2011年  
  • 瀧田怜, 片坐宏一, 北村良実, 石原大助, 大薮進喜, 藤原英明
    日本天文学会年会講演予稿集 2011 2011年  
  • 片坐宏一, 和田武彦, 猿楽祐樹, 左近樹, 小林尚人, 大藪進喜
    日本天文学会年会講演予稿集 2011 2011年  
  • 岡本 美子, 片坐 宏一, 三ツ井 健司, 岡田 則夫
    日本赤外線学会誌 = Journal of the Japan Society of Infraed Science and Technolog 19(1) 65-68 2010年5月30日  

共同研究・競争的資金等の研究課題

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