Kouichiro Nakanishi
Graduate University for Advanced Studies
323 Papers
4.3K Citations
Kouichiro Nakanishi is an academic researcher from Graduate University for Advanced Studies. The author has contributed to research in topics: Galaxy & Star formation. The author has an hindex of 51, co-authored 304 publications. Previous affiliations of Kouichiro Nakanishi include National Institutes of Natural Sciences, Japan & Kitt Peak National Observatory.
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Papers
A radio-to-mm census of star-forming galaxies in protocluster 4C23.56 at z=2.5 : Gas mass and its fraction revealed with ALMA
Minju Lee,Ichi Tanaka,Ryohei Kawabe,Ryohei Kawabe,Kotaro Kohno,Tadayuki Kodama,Masaru Kajisawa,Min S. Yun,Kouichiro Nakanishi,Daisuke Iono,Yoichi Tamura,Yoichi Tamura,Bunyo Hatsukade,Hideki Umehata,Hideki Umehata,Toshiki Saito,Takuma Izumi,Itziar Aretxaga,Ken-ichi Tadaki,Milagros Zeballos,Soh Ikarashi,Grant W. Wilson,David H. Hughes,Rob Ivison,Rob Ivison +24 more
TL;DR: In this article, the gas contents of star-forming galaxies associated with protocluster 4C23 were investigated by using the Atacama Large Millimeter/submillimeter Array (ALMA) with the redshifted CO(3-2) and 1.1 mm dust continuum.
Optical follow-up observations of the ASCA Lynx Deep Survey
Kunihiro Ohta,Masayuki Akiyama,Kouichiro Nakanishi,Toru Yamada,Kiyoshi Hayashida,Tsuneo Kii,Y. Ogasaka +6 more
Abstract: Since the bulk of the energy density of the Cosmic X-ray Background (CXB) resides in the harder energy band than that of the ROSAT band (0.5–2 keV) and since the X-ray sources identified in the ROSAT band have X-ray spectra softer than that of the CXB, investigation of nature of the X-ray sources at the harder energy band is indispensable to solve the origin of the CXB. However, only 2–3% of the CXB in the hard band (2–10 keV) had been resolved into discrete sources (Piccinotti et al. 1982, ApJ 253, 485). We present our preliminary results of optical follow-up observations of the ASCA Lynx deep survey.
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Atacama compact array antennas
TL;DR: The Atacama Compact Array (ACA) as mentioned in this paper is an important element of ALMA and consists of four ACA 12m antennas and twelve ACA 7m antennas, and the science performance of these antennas has been extensively verified at OSF (operation support facility) at an elevation of 2900 m in northern Chile since 2007.
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Isolated Millimeter Flares of Cyg X-3
TL;DR: In this paper, isolated flares in the quiescent phase of Cygnus X-3 were observed at 23, 43, and 86 GHz with the 45m radio telescope at Nobeyama Radio Observatory.
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Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) XII. Extended [C II] Structure (Merger or Outflow) in a z = 6.72 Red Quasar.
Takuma Izumi,Masafusa Onoue,Yoshiki Matsuoka,Michael A. Strauss,Seiji Fujimoto,Hideki Umehata,Masatoshi Imanishi,Taiki Kawamuro,Tohru Nagao,Yoshiki Toba,Kotaro Kohno,Nobunari Kashikawa,Kohei Inayoshi,Toshihiro Kawaguchi,Kazushi Iwasawa,Akio K. Inoue,Tomotsugu Goto,Shunsuke Baba,Malte Schram,Hyewon Suh,Yuichi Harikane,Yoshihiro Ueda,John D. Silverman,Takuya Hashimoto,Yasuhiro Hashimoto,Soh Ikarashi,Daisuke Iono,Chien-Hsiu Lee,Kianhong Lee,Takeo Minezaki,Kouichiro Nakanishi,Suzuka Nakano,Yoichi Tamura,Ji-Jia Tang +33 more
TL;DR: In this article, the authors presented ALMA [C II] 158 $\mu$m line and far-infrared (FIR) emission observations toward HSC J120505.9 (J1205$-$0000) at $z = 6.72$ with the beam size of $\sim 0''.8 \times 0''.5$ (or 4.1 kpc $\times$ 2.6 kpc).
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