井上 昭雄 (イノウエ アキオ)

写真a

所属

理工学術院 先進理工学部

職名

教授(任期付)

メールアドレス

メールアドレス

ホームページ

http://www.obsap.phys.waseda.ac.jp/

学内研究所等 【 表示 / 非表示

  • 2020年
    -
    2022年

    理工学術院総合研究所   兼任研究員

学歴 【 表示 / 非表示

  • 2000年04月
    -
    2003年03月

    京都大学   理学研究科   物理学・宇宙物理学専攻宇宙物理学教室  

  • 1998年04月
    -
    2000年03月

    京都大学   大学院理学研究科   物理学・宇宙物理学専攻宇宙物理学教室  

  • 1994年04月
    -
    1998年03月

    京都大学   理学部  

学位 【 表示 / 非表示

  • 理学修士

  • 京都大学   博士(理学)

経歴 【 表示 / 非表示

  • 2019年04月
    -
    継続中

    早稲田大学   理工学術院   教授(任期付)

  • 2017年04月
    -
    2019年03月

    大阪産業大学   デザイン工学部環境理工学科   准教授

  • 2008年04月
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    2017年03月

    大阪産業大学 教養部 物理 准教授

  • 2005年04月
    -
    2008年03月

    大阪産業大学 教養部 物理 講師

所属学協会 【 表示 / 非表示

  •  
     
     

    日本天文学会

  •  
     
     

    日本惑星科学会

  •  
     
     

    国際天文学連合

  •  
     
     

    American Astronomical Society

  •  
     
     

    理論天文学宇宙物理学懇談会

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研究分野 【 表示 / 非表示

  • 天文学

論文 【 表示 / 非表示

  • AstroSat detection of Lyman continuum emission from a z = 1.42 galaxy

    Kanak Saha, Shyam N. Tandon, Charlotte Simmonds, Anne Verhamme, Abhishek Paswan, Daniel Schaerer, Michael Rutkowski, Anshuman Borgohain, Bruce Elmegreen, Akio K. Inoue, Francoise Combes, Debra Elmegreen, Mieke Paalvast

    Nature Astronomy   4 ( 12 ) 1185 - 1194  2020年12月

     概要を見る

    One of the outstanding problems of current observational cosmology is to understand the nature of sources that produced the bulk of the ionizing radiation after the Cosmic Dark Age. Direct detection of these reionization sources1 is practically infeasible at high redshift (z) due to the steep decline of intergalactic medium transmission2,3. However, a number of low-z analogues emitting Lyman continuum at 900 Å restframe are now detected at z < 0.4 (refs. 4–8) and there are also detections in the range 2.5 < z < 3.5 (refs. 9–14). Here we report the detection of Lyman continuum emission with a high escape fraction (>20%) from a low-mass clumpy galaxy at z = 1.42, in the middle of the redshift range where no detection has been made before and near the peak of the cosmic star-formation history15. The observation was made in the Hubble Extreme Deep Field16 by the wide-field Ultraviolet Imaging Telescope17 onboard AstroSat18. This detection of extreme ultraviolet radiation from a distant galaxy at a restframe wavelength of 600 Å opens up a new window to constrain the shape of the ionization spectrum. Further observations with AstroSat should substantially increase the sample of Lyman-continuum-leaking galaxies at cosmic noon.

    DOI

  • CHORUS. I. Cosmic HydrOgen reionization unveiled with subaru: Overview

    Akio K. Inoue, Satoshi Yamanaka, Masami Ouchi, Ikuru Iwata, Kazuhiro Shimasaku, Yoshiaki Taniguchi, Tohru Nagao, Nobunari Kashikawa, Yoshiaki Ono, Ken Mawatari, Takatoshi Shibuya, Masao Hayashi, Hiroyuki Ikeda, Haibin Zhang, Yongming Liang, Chien Hsiu Lee, Miftahul Hilmi, Satoshi Kikuta, Haruka Kusakabe, Hisanori Furusawa, Tomoki Hayashino, Masaru Kajisawa, Yuichi Matsuda, Kimihiko Nakajima, Rieko Momose, Yuichi Harikane, Tomoki Saito, Tadayuki Kodama, Shotaro Kikuchihara, Masanori Iye, Tomotsugu Goto

    Publications of the Astronomical Society of Japan   72 ( 6 )  2020年12月

     概要を見る

    To determine the dominant sources for cosmic reionization, the evolution history of the global ionizing fraction, and the topology of the ionized regions, we have conducted a deep imaging survey using four narrow-band (NB) and one intermediate-band (IB) filters on the Subaru/Hyper Suprime-Cam (HSC), called Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS). The central wavelengths and full-widths-at-half-maximum of the CHORUS filters are, respectively, 386.2 nm and 5.5 nm for NB387, 526.0 nm and 7.9 nm for NB527, 717.1 nm and 11.1 nm for NB718, 946.2 nm and 33.0 nm for IB945, and 971.2 nm and 11.2 nm for NB973. This combination, including NB921 (921.5 nm and 13.5 nm) from the Subaru Strategic Program with HSC (HSC SSP), is carefully designed, as if they were playing a chorus, to observe multiple spectral features simultaneously, such as Lyman continuum, Lyα, C IV, and He II for z = 2-7. The observing field is the same as that of the deepest footprint of the HSC SSP in the COSMOS field and its effective area is about 1.6 deg2. We present an overview of the CHORUS project, which includes descriptions of the filter design philosophy, observations and data reduction, multiband photometric catalogs, assessments of the imaging quality, measurements of the number counts, and example use cases for the data. All the imaging data, photometric catalogs, masked pixel images, data of limiting magnitudes and point spread functions, results of completeness simulations, and source number counts are publicly available through the HSC SSP database.

    DOI

  • Balmer Break Galaxy Candidates at z~6: a Potential View on the Star-Formation Activity at z>14

    Ken Mawatari, Akio K. Inoue, Takuya Hashimoto, John Silverman, Masaru Kajisawa, Satoshi Yamanaka, Toru Yamada, Iary Davidzon, Peter Capak, Lihwai Lin, Bau-Ching Hsieh, Yoshiaki Taniguchi, Masayuki Tanaka, Yoshiaki Ono, Yuichi Harikane, Yuma Sugahara, Seiji Fujimoto, Tohru Nagao

    The Astrophysical Journal   889 ( 2 ) 137  2020年  [査読有り]

     概要を見る

    We search for galaxies with a strong Balmer break (Balmer break galaxies; BBGs) at z ∼ 6 over a 0.41 deg2 effective area in the COSMOS field. Based on rich imaging data, including data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA), three candidates are identified by their extremely red K-[3.6] colors, as well as by nondetection in the X-ray, optical, far-infrared, and radio bands. The nondetection in the deep ALMA observations suggests that they are not dusty galaxies but BBGs at z ∼ 6, although contamination from active galactic nuclei at z ∼ 0 cannot be completely ruled out for the moment. Our spectral energy distribution analyses reveal that the BBG candidates at z ∼ 6 have stellar masses of ≈5 × 1010 M o&dot; dominated by old stellar populations with ages of ⪆ 700 Myr. Assuming that all three candidates are real BBGs at z ∼ 6, we estimate the stellar mass density to be 2.4-1.3 +2.3× 10-4,M Mpc-3. This is consistent with an extrapolation from the lower-redshift measurements. The onset of star formation in the three BBG candidates is expected to be several hundred million yr before the observed epoch of z ∼ 6. We estimate the star formation rate density (SFRD) contributed by progenitors of the BBGs to be 2.4-12 × 10-5 M o&dot; yr-1 Mpc-3 at z > 14 (99.7% confidence range). Our result suggests a smooth evolution of the SFRD beyond z = 8.

    DOI

  • "Big Three Dragons": a z = 7.15 Lyman BreakGalaxy Detected in [OIII] 88 $μ$m, [CII] 158 $μ$m, and Dust Continuum with ALMA

    Takuya Hashimoto, Akio K. Inoue, Ken Mawatari, Yoichi Tamura, Hiroshi Matsuo, Hisanori Furusawa, Yuichi Harikane, Takatoshi Shibuya, Kirsten K. Knudsen, Kotaro Kohno, Yoshiaki Ono, Erik Zackrisson, Takashi Okamoto, Nobunari Kashikawa, Pascal A. Oesch, Masami Ouchi, Kazuaki Ota, Ikkoh Shimizu, Yoshiaki Taniguchi, Hideki Umehata, Darach Watson

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   71 ( 4 )  2018年06月  [査読有り]

     概要を見る

    We present new ALMA observations and physical properties of a Lyman Break
    Galaxy at z=7.15. Our target, B14-65666, has a bright ultra-violet (UV)
    absolute magnitude, $M_{\rm UV}\approx-22.4$, and has been spectroscopically
    identified in Ly$\alpha$ with a small rest-frame equivalent width of $\approx4$
    \AA. Previous HST image has shown that the target is comprised of two spatially
    separated clumps in the rest-frame UV. With ALMA, we have newly detected
    spatially resolved [OIII] 88 $\mu$m, [CII] 158 $\mu$m, and their underlying
    dust continuum emission. In the whole system of B14-65666, the [OIII] and [CII]
    lines have consistent redshifts of $7.1520\pm0.0003$, and the [OIII]
    luminosity, $(34.4\pm4.1)\times10^{8}L_{\rm \odot}$, is about three times
    higher than the [CII] luminosity, $(11.0\pm1.4)\times10^{8}L_{\rm \odot}$. With
    our two continuum flux densities, the dust temperature is constrained to be
    $T_{\rm d}\approx50-60$ K under the assumption of the dust emissivity index of
    $\beta_{\rm d}=2.0-1.5$, leading to a large total infrared luminosity of
    $L_{\rm TIR}\approx1\times10^{12}L_{\rm \odot}$. Owing to our high spatial
    resolution data, we show that the [OIII] and [CII] emission can be spatially
    decomposed into two clumps associated with the two rest-frame UV clumps whose
    spectra are kinematically separated by $\approx200$ km s$^{-1}$. We also find
    these two clumps have comparable UV, infrared, [OIII], and [CII] luminosities.
    Based on these results, we argue that B14-65666 is a starburst galaxy induced
    by a major-merger. The merger interpretation is also supported by the large
    specific star-formation rate (defined as the star-formation rate per unit
    stellar mass), sSFR$=260^{+119}_{-57}$ Gyr$^{-1}$, inferred from our SED
    fitting. Probably, a strong UV radiation field caused by intense star formation
    contributes to its high dust temperature and the [OIII]-to-[CII] luminosity
    ratio.

    DOI

  • SILVERRUSH. VI. A simulation of Lyα emitters in the reionization epoch and a comparison with Subaru Hyper Suprime-Cam survey early data

    Inoue, Akio K, Hasegawa, Kenji, Ishiyama, Tomoaki, Yajima, Hidenobu, Shimizu, Ikkoh, Umemura, Masayuki, Konno, Akira, Harikane, Yuichi, Shibuya, Takatoshi, Ouchi, Masami, Shimasaku, Kazuhiro, Ono, Yoshiaki, Kusakabe, Haruka, Higuchi, Ryo, Lee, Chien-Hsiu

    Publications of the Astronomical Society of Japan   70 ( 3 ) id. 55, 30 pp.  2018年06月  [査読有り]

    DOI

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書籍等出版物 【 表示 / 非表示

  • 新天文学事典

    井上昭雄, 釜谷秀幸( 担当: 共著)

    講談社  2013年03月

     概要を見る

    講談社ブルーバックスシリーズで出版された最新の天文学の解説書。『第13章星間物質』では、星間空間に存在するガス、宇宙塵、磁場、宇宙線、放射場などの状態や物理・化学過程について、基礎から最新の知見まで概説した。

Misc 【 表示 / 非表示

  • WISH for deep and wide NIR surveys

    Toru Yamada, Ikuru Iwata, Makiko Ando, Mamoru Doi, Tomotsugu Goto, Yuji Ikeda, Masatoshi Imanishi, Akio K. Inoue, Satoru Iwamura, Nobuyuki Kawai, Masakazu A.R. Kobayashi, Tadayuki Kodama, Yutaka Komiyama, Mariko Kubo, Hideo Matsuhara, Ken Mawatari, Yoshiki Matsuoka, Tomoki Morokuma, Hidehiko Nakaya, Kouji Ohta, Atsushi Okamoto, Sinki Oyabu, Yoichi Sato, Hiroyuki Sugita, Ryo Tsutsui, Chihiro Tokoku, Jun Toshikawa, Saku Tsuneta, Takehiko Wada, Kiyoto Yabe, Naoki Yasuda, Daisuke Yonetoku

    Proceedings of SPIE - The International Society for Optical Engineering   8442   84421A  2012年

     概要を見る

    WISH, Wide-field Imaging Surveyor for High-redshiftt, is a space mission concept to conduct very deep and widefield surveys at near infrared wavelength at 1-5μm to study the properties of galaxies at very high redshift beyond the epoch of cosmic reionization. The concept has been developed and studied since 2008 to be proposed for future JAXA/ISAS mission. WISH has a 1.5m-diameter primary mirror and a wide-field imager covering 850 arcmin2. The pixel scale is 0.155 arcsec for 18μm pitch, which properly samples the diffraction-limited image at 1.5μm. The main program is Ultra Deep Survey (UDS) covering 100 deg2 down to 28AB mag at least in five broad bands. We expect to detect &gt
    104 galaxies at z=8-9, 10 3-104 galaxies at z=11-12, and 50-100 galaxies at z&gt
    14, many of which can be feasible targets for deep spectroscopy with Extremely Large Telescopes. With recurrent deep observations, detection and light curve monitoring for type-Ia SNe in rest-frame infrared wavelength is also conducted, which is another main science goal of the mission. During the in-orbit 5 years observations, we expect to detect and monitor &gt
    2000 type-Ia SNe up to z̃2. WISH also conducts Ultra Wide Survey, covering 1000deg2 down to 24-25AB mag as well as Extreme Survey, covering a limited number of fields of view down to 29-30AB mag. We here report the progress of the WISH project including the basic telescope and satellite design as well as the results of the test for a proto-model of the flip-type filter exchanger which works robustly near 100K. © 2012 SPIE.

    DOI

  • WISH: Wide-field imaging surveyor for high-redshift

    Toru Yamada, Mamoru Doi, Tomotsugu Gotc, Yuji Ikeda, Masatoshi Imanishi, Akio Inoue, Satoru Iwamura, Ikuru Iwata, Nobuyuki Kawai, Masakazu A.R. Kobayashie, Tadayuki Kodama, Yutaka Komiyama, Hideo Matsuhara, Yoshiki Matsuoka, Tomoki Morokuma, Kouji Ohta, Shinki Oyabu, Yoichi Sato, Hiroyuki Sugita, Ryo Tsutsui, Chihiro Tokoku, Saku Tsuneta, Takehiko Wada, Kiyoto Yabe, Naoki Yasuda, Daisuke Yonetoku

    Proceedings of SPIE - The International Society for Optical Engineering   7731   77311Q  2010年

     概要を見る

    WISH is a new space science mission concept whose primary goal is to study the first galaxies in the early universe. We will launch a 1.5m telescope equipped with 1000 arcmin2 wide-field NIR camera by late 2010's in order to conduct unique ultra-deep and wide-area sky surveys at 1-5 micron. The primary science goal of WISH mission is pushing the high-redshift frontier beyond the epoch of reionization by utilizing its unique imaging capability and the dedicated survey strategy. We expect to detect ∼ 104 galaxies at z=8-9, ∼ 3-6×103 galaxies at z=11-12, and ∼50-100 galaxies at z=14-17 within about 5 years of the planned mission life time. It is worth mentioning that a large fraction of these objects may be bright enough for the spectroscopic observations with the extremely large telescopes. By adopting the optimized strategy for the recurrent observations to reach the depth, we also use the surveys to detect transient objects. Type Ia Supernova cosmology is thus another important primary goal of WISH. A unique optical layout has been developed to achieve the diffraction-limited imaging at 1-5micron over the required large area. Cooling the mirror and telescope to ∼100K is needed to achieve the zodiacal light limited imaging and WISH will achieve the required temperature by passive cooling in the stable thermal environment at the orbit near Sun-Earth L2. We are conducting the conceptual studies and development for the important components of WISH including the exchange mechanism for the wide-field filters as well as the primary mirror fixation. © 2010 SPIE.

    DOI

  • 銀河からの電離光子脱出率の進化と宇宙再電離

    井上昭雄

    大阪産業大学論集 自然科学編   ( 117 ) 1 - 16  2006年02月  [査読有り]

    記事・総説・解説・論説等(大学・研究所紀要)  

     概要を見る

    ビッグバンの38万年後にいったん中性化した宇宙が、その後数億年程度で再び電離状態になる、宇宙再電離過程についての研究。形成途中の若い銀河からの電離光子供給量が、現在の宇宙に比べて過去の宇宙、つまり再電離期に近い時期ほど多かった可能性を初めて指摘した。

共同研究・競争的資金等の研究課題 【 表示 / 非表示

  • すばるHSC狭帯域深宇宙探査で暴く宇宙再電離:CHORUSプロジェクト

    研究期間:

    2017年04月
    -
    2021年03月
     

  • すばるHSC観測と宇宙再電離大規模シミュレーションによる電離度マップの描画

    研究期間:

    2014年04月
    -
    2017年03月
     

    井上 昭雄

    担当区分: 研究代表者

  • 宇宙再電離完了期z=6.6における電離度空間分布の描画と再電離光源の探究

    研究期間:

    2011年04月
    -
    2015年03月
     

  • 銀河の実効的ダスト減光曲線進化とその観測的検証

    研究期間:

    2007年
    -
    2010年
     

  • 銀河の実効的ダスト減光曲線進化の研究

    研究期間:

    2006年
    -
    2007年
     

講演・口頭発表等 【 表示 / 非表示

  • Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS)

    井上昭雄, 他CHORUSメンバー

    日本天文学会2016年春季年会   (首都大学東京) 

    発表年月: 2016年03月

  • 銀河間空間におけるダストサイズ分布

    井上昭雄

    サイズ分布ビッグピクチャー研究会   (千葉工業大学スカイツリーキャンパス) 

    発表年月: 2016年02月

  • 銀河形成・宇宙再電離と高赤方偏移の超巨大ブラックホール

    井上昭雄, 長峯健太郎

    「超巨大ブラックホール研究推進連絡会」第3回ワークショップ   (甲南大学) 

    発表年月: 2015年10月

  • 赤方偏移9を超える重力レンズ銀河候補からのCIII]1909輝線強度予想

    井上昭雄, 清水一紘

    日本天文学会2015年秋季年会   (甲南大学) 

    発表年月: 2015年09月

  • Prediction of emission line fluxes of gravitationally lensed very high-z galaxies

    Inoue, A. K, Shimizu, I, Okamoto, T, Yoshida, N, Matsuo, H, Tamura, Y

    IAU General Assembly, Meeting #29, id.2246421   (Honolulu) 

    発表年月: 2015年08月

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