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  2. Takao Nakagawa

Takao Nakagawa

  (中川 貴雄)

Profile Information

Affiliation
教授, 宇宙科学研究所・宇宙物理学研究系, 国立研究開発法人宇宙航空研究開発機構
Professor, Graduate School of Science, Department of Physics, The University of Tokyo
Degree
(BLANK)(The University of Tokyo)
(BLANK)(The University of Tokyo)
J-GLOBAL ID
200901060914122911
researchmap Member ID
1000363024
External link

Research Interests

 5

Research Areas

 1

Committee Memberships

 3

Awards

 2

Papers

 382
  • Kosei Matsumoto, Peter Camps, Maarten Baes, Frederik De Ceuster, Keiichi Wada, Takao Nakagawa, Kentaro Nagamine
    Astronomy & Astrophysics, Oct, 2023  
  • Naoki Isobe, Hiroshi Nagai, Motoki Kino, Shunsuke Baba, Takao Nakagawa, Yuji Sunada, Makoto Tashiro
    The Astrophysical Journal, Aug 1, 2023  
  • Youichi Ohyama, Shusuke Onishi, Takao Nakagawa, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Shunsuke Baba, Kazushi Sakamoto
    The Astrophysical Journal, Jul 1, 2023  
  • Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun’ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
    The Astronomical Journal, 165(4) 162-162, Mar 17, 2023  
    Abstract The Subaru telescope is currently performing a strategic program (SSP) using the high-precision near-infrared (NIR) spectrometer IRD to search for exoplanets around nearby mid/late M dwarfs via radial velocity (RV) monitoring. As part of the observing strategy for the exoplanet survey, signatures of massive companions such as RV trends are used to reduce the priority of those stars. However, this RV information remains useful for studying the stellar multiplicity of nearby M dwarfs. To search for companions around such “deprioritized” M dwarfs, we observed 14 IRD-SSP targets using Keck/NIRC2 with pyramid wave-front sensing at NIR wavelengths, leading to high sensitivity to substellar-mass companions within a few arcseconds. We detected two new companions (LSPM J1002+1459 B and LSPM J2204+1505 B) and two new candidates that are likely companions (LSPM J0825+6902 B and LSPM J1645+0444 B), as well as one known companion. Including two known companions resolved by the IRD fiber injection module camera, we detected seven (four new) companions at projected separations between ∼2 and 20 au in total. A comparison of the colors with the spectral library suggests that LSPM J2204+1505 B and LSPM J0825+6902 B are located at the boundary between late M and early L spectral types. Our deep high-contrast imaging for targets where no bright companions were resolved did not reveal any additional companion candidates. The NIRC2 detection limits could constrain potential substellar-mass companions (∼10–75 MJup) at 10 au or further. The failure with Keck/NIRC2 around the IRD-SSP stars having significant RV trends makes these objects promising targets for further RV monitoring or deeper imaging with the James Webb Space Telescope to search for smaller-mass companions below the NIRC2 detection limits.
  • Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
    The Astronomical Journal, Feb 1, 2023  
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Misc.

 674
  • 芝井広, 奥田治之, 中川貴雄, 山下由香利, 舞原俊憲, 福井康雄, 小林行泰, 広本宣久, LOW F J
    日本天文学会年会講演予稿集, 1991, 1991  
  • 望月賢治, 山下由香利, 土井靖生, 中川貴雄, 奥田治之, 矢島信之, 芝井広, 広本宣久
    日本天文学会年会講演予稿集, 1991, 1991  
  • 山下由香利, 中川貴雄, 奥田治之, 矢島信之, 土井靖生, 西村徹朗, 芝井広, LOW F J
    日本天文学会年会講演予稿集, 1991, 1991  
  • 中川貴雄, 奥田治之, 芝井広, 松原英雄, 小林行泰, 広本宣久
    日本天文学会年会講演予稿集, 1991, 1991  
  • 山下由香利, 中川貴雄, 芝井広, 奥田治之
    日本天文学会年会講演予稿集, 1991, 1991  
  • 芝井広, 矢島信之, 中川貴雄, 奥田治之
    大気球シンポジウム, 1990, 1991  
  • Takao Nakagawa, Tetsuya Nagata, Hideo Matsuhara, Haruyuki Okuda, Hiroshi Shibai, Saeko S. Hayashi
    Astrophysical Journal, 351(2) 573-577, Mar 10, 1990  
    Exceptionally high degrees (up to ∼100%) of polarization was observed in the L′ band (3.8 μm) toward the NGC 6334 V bipolar nebula. The observed symmetric polarization pattern indicates that the nebula is a reflection nebula consisting of two lobes illuminated by a central obscured star. The measured distribution of high degrees of polarization requires that one of the lobes consist of a lemon-shaped cavity which scatters light mainly at its surface, whereas a conical cavity model is appropriate for the other lobe. This asymmetry of the lobes is probably due to a density gradient in the ambient cloud material in this region.
  • H SHIBAI, H OKUDA, T NAKAGAWA, H MATSUHARA, T MAIHARA, K MIZUTANI, Y KOBAYASHI, N HIROMOTO, T NISHIMURA, FJ LOW
    FROM GROUND-BASED TO SPACE-BORNE SUB-MM ASTRONOMY, 314 141-147, 1990  
  • 中川貴雄, 奥田治之, 芝井広, 矢島信之, 並木道義, 水谷耕平, 山下由香利, 土井靖生, 石丸友里
    日本天文学会年会講演予稿集, 1990(shuki), 1990  
  • 芝井広, 奥田治之, 中川貴雄, 舞原俊憲, 水谷耕平, 松原英雄, 小林行泰, 広本宣久, LOW F J, 西村徹郎
    日本天文学会年会講演予稿集, 1990(shuki), 1990  
  • 芝井広, 奥田治之, 中川貴雄, 松原英雄, 舞原俊憲, 水谷耕平, 小林行泰, 広本宣久, 西村徹郎
    大気球シンポジウム, 1989, 1990  
  • 広本宣久, 板部敏和, 秋葉誠, 奥田治之, 芝井広, 中川貴雄, 松原英雄
    搭載機器基礎開発成果報告書, 3, 1990  
  • 広本宣久, 板部敏和, 秋葉誠, 芝井広, 奥田治之, 中川貴雄, 松原英雄
    宇宙放射線シンポジウム, 1989, 1990  
  • 中川貴雄, 奥田治之, 村上浩, 芝井広, 矢島信之, 太田茂雄, 並木道義, 松原英雄, 山下由香利
    大気球シンポジウム, 1989, 1990  
  • 芝井宏, 奥田治之, 中川貴雄, 松原英雄, 広本宣久, RICHARDS P L
    宇宙放射線シンポジウム, 1989, 1990  
  • 中川貴雄, 奥田治之, 村上浩, 芝井広, 矢島信之, 太田茂雄, 並木道義, 松原英雄, 山下由香利
    宇宙放射線シンポジウム, 1989, 1990  
  • 中川貴雄, 奥田治之, 芝井広, 松原英雄, 舞原俊憲, 水谷耕平, LOW F J, 小林行泰, 広本宣久
    宇宙科学研究所報告 特集, (25) p253-273, 1990  
    Interstellar far-ultraviolet radiation (FUV : 912<λ<2000A) dominates the heating and many important aspects of physics and chemistry in some interstellar neutral regions. These regions are called "photodissociation regions." We have made far-infrared spectroscopic observations of many photodissociation regions with a 50cm Balloon-borne Infrared Telescope (BIRT) and a liquid helium cooled Fabry-Perot spectrometer. We also adopted a frequency switching method to observe diffuse compoents efficiently. The spectral lines we observed are [CII] (^2P_<3/2>-^2P_<1/2>. 158μm) and [OI] (^3P_1-^3P_2,63μm), both of which are the most important coolants in photodissociation regions. We have observed many kinds of photodissociation regions, including active star-forming regions (M17 and NGC6334), central regions of our Galaxy, and wide regions along the Galactic plane. Our observations showed that (1) photodissociation regions are very clumpy and that FUV penetrates deep into clouds, (2) photodissociation regions are ubiquitous, and (3) photodissociation regions are not minor interstellar components but their total mass in our Galaxy amounts to 40% of that of molecular gas.
  • NAKAGAWA Takao, OKUDA Haruyuki, SHIBAI Hiroshi, MATSUHARA Hideo, MAIHARA Toshinori, MIZUTANI Kohei, Low F. J., NISHIMURA Tetsuo, KOBAYASHI Yukiyasu, HIROMOTO Norihisa
    24(24) p129-137, Dec, 1989  
    We have made spectrocopic observations of the farinfrared [CII] (^2P_<3/2>&xmap;^2P_<1/2>, λ=157.74μm) line toward an active star-forming complex NGC 6334 with a balloon-borne 50cm telescope and a liquid-Helium cooled Fabry-Perot spectrometer. We have also obtained a two-dimensional map of the NGC 6334 complex by utilizing the newly developed frequency switching method. Strong [CII] emission has been detected throughout the region we have observed. Even a region (source V) with no compact HII region has been found to be a strong emitter of the [CII] line. We propose two hypotheses to explain the emission from source V as follows : (1) photodissociation regions around the source had evolved more rapidly than corresponding HII regions, and (2) the region around the source is very rich in B-type stars, which contribute significantly to [CII] emission but produce negligible HII regions.
  • MATSUHARA H., NAKAGAWA T., SHIBAI H., OKUDA H., MIZUTANI K., MAIHARA T., KOBAYASHI Y., HIROMOTO N., NISHIMURA T., Low F. J.
    24(24) p139-147, Dec, 1989  
    Balloon observations of [CII] 158μm and [OI] 63μm from the M17 HII region and the molecular cloud complex are presented. Spatial distribution and energetics of the CII region are discussed. Around the M17 HII region, [OI] 63μm significantly contributes to the cooling of the CII region. Heating due to photoelectric effect of dust grains illuminated by the intence UV radiation can compensate for the cooling due to [CII] and [OI] lines. The CII region extends far beyond the HII region, which indicates the clumpy structure of the CII region. The existence of low-brightness, diffuse [CII] emission component toward M17 SW molecular cloud has been revealed. Distribution of the [CII] emission is quite similar to that of ^<12>CO J=1&xmap;0 emission. Possible energy source of the [CII] emission is discussed. Ratio of the [CII] luminosity to the total far-infrared luminosity of this diffuse component has been found to exceed that of the intence [CII] emission component around the HII region.
  • SHIBAI Hiroshi, OKUDA Haruyuki, NAKAGAWA Takao, MATSUHARA Hideo, MAIHARA Toshinori, MIZUTANI Kohei, KOBAYASHI Yukiyasu, HIROMOTO Norihisa, LOW Frank J., NISHIMURA Tetsuo
    24(24) p149-162, Dec, 1989  
    Diffuse [C II] line emission at 157.74μm has been observed in an extensive region along the Galactic plane, using a ballon-borne infrared telescope incorporated with a liquid helium cooled Fabry-Perot spectrometer. Strong emission has been ubiquitously detected all over the region between 1=30°and 51°. Most of the emission seems to be diffuse and unassociated with discrete HII regions. The longitude profile of the integrated [C II] intensity distribution is similar to those of IRAS 100μm and ^<12>CO (1-0) but not to that of HI 21cm. The large-scale diffuse [C II] emission probably comes from surfaces of molecular clouds which from diffuse photodissociation regions. The total [C II] luminosity of the Galaxy amounts to 2.6×10^7 L_&ofcir; which corresponds to about 0.35% of the total far-infrared luminosity.
  • T NAKAGAWA, T NAGATA, TR GEBALLE, H OKUDA, H SHIBAI, H MATSUHARA
    ASTROPHYSICAL JOURNAL, 340(2) 729-738, May, 1989  
  • SHIBAI H., OKUDA H., NAKAGAWA T., MATSUHARA H., MAIHARA T., MIZUTANI K., Low F.J., NISHIMURA T., KOBAYASHI Y., TAKAMI H., HIROMOTO N.
    23(23) p69-76, Mar, 1989  
    Far-infrared spectroscopic observations have been made using a 50cm balloon-borne infrared telescope, a superfluid helium cooled Fabry-Perot spectrometer, and a frequency switching method, which is a newly developped observational technique. Remarkable two-dimensional [CII] line intensity maps constructed from the data show us that the [CII] 158μm line is strongly emitted not only from the photodissociation regions but also from their surrounding regions and from general region of the Galactic Plane. This fact indicates singly ionized carbon ions and carbon ioinizing UV photons should be abundantly distributed in interstellar clouds of the Galactic Plane. Since the energy emitted in form of the [CII] 158μm line can reach up to 0.5% of the total energy output of the clouds, the [CII] line must be one of the dominant coolants of the interstellar cloud.
  • 廣本 宣久, 板部 敏和, 有賀 規, 猪股 英行, 奥田 治之, 松原 英雄, 芝井 広, 中川 貴雄, 斉藤 稔
    情報通信研究機構研究報告, 35(175) 143-156, 1989  
  • 芝井広, 奥田治之, 舞原俊憲, 高見英樹, 広本宣久, 中川貴雄, 小林行泰, THOMAS J A, SOOD R
    宇宙科学研究所報告 特集, (17) 91-99, 1986  
    Far-infrared H_2O emission spectra of the upper atmosphere have been obtained during a balloon flight in Alice Springs, Australia. Analyses show that the emission features of the telluric H_2O are fitted by a model atmosphere of 245K in mean temperature and of 1.7×10^<18>cm^<-2> in H_2O column density. We have also made an assessment for the telluric H_2O absorption via this model, thus anabling a correction of the observed astronmical spectra.

Professional Memberships

 3

Research Projects

 49
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● 専任大学名

 1
  • Affiliation (university)
    東京大学（University of Tokyo)
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