2022/09/22 更新

写真a

サノ ケイ
佐野 圭
SANO Kei
Scopus 論文情報  
総論文数: 0  総Citation: 0  h-index: 7

Citation Countは当該年に発表した論文の被引用数

所属
大学院工学研究院 宇宙システム工学研究系
職名
助教
研究室住所
福岡県北九州市戸畑区仙水町1-1
外部リンク

研究キーワード

  • 観測的宇宙論

  • 宇宙物理学

  • 宇宙史

  • 宇宙背景放射

  • 銀河形成

  • 初期宇宙

  • 初代星

  • ブラックホール

  • 銀河間物質

  • 銀河系

  • 星間輻射場

  • 星間塵

  • 惑星間塵

  • 黄道光

  • 光散乱

  • ガンマ線バースト

  • 突発天体

  • データ解析

  • 宇宙システム

  • 観測ロケット

  • 小型衛星

  • 深宇宙探査機

  • 観測装置

  • 望遠鏡

  • 光学設計

  • 分光器

  • 熱構造

  • 機械設計

  • 振動

  • 金属腐食

  • 光赤外線天文学

研究分野

  • 自然科学一般 / 天文学

出身学校

  • 2012年03月   東京大学   理学部   天文学科   卒業   日本国

出身大学院

  • 2017年03月   東京大学   理学系研究科   天文学専攻   博士課程・博士後期課程   修了   日本国

取得学位

  • 東京大学  -  博士(理学)   2017年03月

学内職務経歴

  • 2021年01月 - 現在   九州工業大学   大学院工学研究院   宇宙システム工学研究系     助教

学外略歴

  • 2019年04月 - 2020年12月   金沢大学   理工研究域 数物科学系 宇宙物理学研究室   日本学術振興会特別研究員   日本国

  • 2017年04月 - 2019年03月   関西学院大学   理工学研究科   研究員   日本国

所属学会・委員会

  • 2021年06月 - 2023年05月   日本天文学会 キャリア支援委員会   日本国

  •   日本天文学会   日本国

研究経歴

  • 可視光近赤外線宇宙背景放射観測用超小型衛星の開発

    研究期間: 2021年04月  -  現在

  • 望遠鏡の表面コーティングに関する研究

    金属製望遠鏡、金属コーティング

    研究期間: 2020年04月  -  現在

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    経年劣化の少ない望遠鏡のコーティング方法を調査する。

  • 衛星搭載用赤外線望遠鏡の開発

    天文衛星、望遠鏡

    研究期間: 2019年04月  -  現在

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    将来の天文衛星に搭載する赤外線望遠鏡を開発する。

  • 深宇宙探査機搭載用観測装置の開発

    深宇宙探査機、観測装置

    研究期間: 2018年04月  -  現在

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    深宇宙で稼働予定の探査機に搭載する観測装置を開発する。

  • 黄道光観測による惑星間塵の研究

    黄道光、惑星間塵

    研究期間: 2014年04月  -  現在

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    可視光や赤外線で黄道光を観測することにより、太陽系内の惑星間塵の性質を研究する。

  • 観測ロケットによる宇宙赤外線背景放射の観測

    観測ロケット、宇宙赤外線背景放射、望遠鏡

    研究期間: 2014年04月  -  現在

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    観測ロケットを用いて宇宙空間から宇宙背景放射の観測を実施するために、搭載する観測装置を開発する。

  • 衛星観測データによる宇宙赤外線背景放射の研究

    赤外線衛星、宇宙背景放射

    研究期間: 2012年04月  -  現在

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    赤外線衛星観測データを解析し、宇宙赤外線背景放射の測定およびその起源を探究する。

▼全件表示

論文

  • The isotropic interplanetary dust cloud and near-infrared extragalactic background light observed with COBE/DIRBE 査読有り

    Sano K., Matsuura S., Yomo K., Takahashi A.

    Astrophysical Journal   901 ( 2 )   2020年10月

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    担当区分:筆頭著者   記述言語:英語   掲載種別:研究論文(学術雑誌)

    © 2020. The American Astronomical Society. All rights reserved.. We report observation of isotropic interplanetary dust (IPD) by analyzing the infrared (IR) maps of the Diffuse Infrared Background Experiment (DIRBE) on board the Cosmic Background Explorer (COBE) spacecraft. To search for the isotropic IPD, we perform new analysis in terms of the solar elongation angle (), because we expect the zodiacal light (ZL) intensity from the isotropic IPD to decrease as a function of . We use the DIRBE weekly averaged maps covering 64° ≲ ≲ 124° and inspect the dependence of residual intensity after subtracting conventional ZL components. We find the dependence of the residuals, indicating the presence of the isotropic IPD. However, the mid-IR dependence is different from that of the isotropic IPD model at ⪆ 90°, where the residual intensity increases as a function of . To explain the observed dependence, we assume a spheroidal IPD cloud showing higher density farther away from the Sun. We estimate the intensity of the near-IR extragalactic background light (EBL) by subtracting the spheroidal component, assuming the spectral energy distribution from the residual brightness at 12 μm. The EBL intensity is derived as 45-8+11, 21-4+3, and 15 ± 3, nWm-2, sr-1 at 1.25, 2.2, and 3.5 μm, respectively. The EBL is still a few times larger than the integrated light of normal galaxies, suggesting the existence of unaccounted-for extragalactic sources.

    DOI: 10.3847/1538-4357/abad3d

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85092533746&origin=inward

  • Spectral study of scattered light by interstellar dust grains 査読有り

    Sano K.

    Proceedings of the International Astronomical Union   15 ( S341 )   302 - 303   2019年01月

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    担当区分:筆頭著者   記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    Interstellar dust is traced by not only thermal emission but also scattered light. The scattered light spectrum observed from ultraviolet (UV) to near-infrared (IR) is useful to constrain some dust properties, such as size distribution, albedo, and composition. Milky Way Galaxy is a unique environment to observe the diffuse scattered light because we can extract it by removing the contribution of starlight. We have observed the UV to near-IR scattered light with space instruments, including Diffuse Infrared Background Experiment (DIRBE), Hubble Space Telescope (HST), and Multi-purpose Infra-Red Imaging System (MIRIS). The scattered light spectrum is marginally consistent with prediction from a recent dust model including carbonaceous and silicate grains with polycyclic aromatic hydrocarbon (PAH). Based on the MIRIS observation of a diffuse cloud, we compare the scattered light color with the dust model with or without grains larger than 1 micrometer. The result shows that the color is consistent with the model without the large grains, which is consistent with recent simulations of dust growth in low-density regions. However, some observations have shown the spectral excess at ∼ 0.6 micrometer wavelength, suggesting the presence of extended red emission (ERE) which cannot be explained by the conventional dust model.

    DOI: 10.1017/S1743921319002990

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85106795356&origin=inward

  • Galactic Latitude Dependence of Near-infrared Diffuse Galactic Light: Thermal emission or scattered light? 査読有り

    Sano K., Matsuura S.

    Astrophysical Journal   849 ( 1 )   2017年11月

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    担当区分:筆頭著者   記述言語:英語   掲載種別:研究論文(学術雑誌)

    © 2017. The American Astronomical Society. All rights reserved. Near-infrared (IR) diffuse Galactic light (DGL) consists of scattered light and thermal emission from interstellar dust grains illuminated by the interstellar radiation field (ISRF). At 1.25 and 2.2 mm, a recent observational study shows that intensity ratios of the DGL to interstellar 100 mm dust emission steeply decrease toward high Galactic latitudes (b). In this paper, we investigate the origin(s) of the b-dependence on the basis of models of thermal emission and scattered light. Combining a thermal emission model with the regional variation of the polycyclic aromatic hydrocarbon abundance observed with Planck, we show that the contribution of the near-IR thermal emission component to the observed DGL is lower than ~20%. We also examine the b-dependence of the scattered light, assuming a plane-parallel Galaxy with smooth distributions of the ISRF and dust density along the vertical direction, and assuming a scattering phase function according to a recently developed model of interstellar dust. We normalize the scattered light intensity to the 100 mm intensity corrected for deviation from the cosecant-b law according to the Planck observation. As the result, the present model that considers the b-dependence of dust and the ISRF properties can account for the observed b-dependence of the near-IR DGL. However, the uncertainty in the correction for the 100 mm emission is large, and other normalizing quantities may be appropriate for a more robust analysis of the DGL.

    DOI: 10.3847/1538-4357/aa906c

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85064386456&origin=inward

  • FIRST DETECTION OF GALACTIC LATITUDE DEPENDENCE OF NEAR-INFRARED DIFFUSE GALACTIC LIGHT FROM DIRBE RENALYSIS 査読有り

    Sano K., Matsuura S., Tsumura K., Arai T., Shirahata M., Onishi Y.

    Astrophysical Journal Letters   821 ( 1 )   2016年04月

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    担当区分:筆頭著者   記述言語:英語   掲載種別:研究論文(学術雑誌)

    © 2016. The American Astronomical Society. All rights reserved. Observational study on near-infrared (IR) scattering properties of interstellar dust grains has been limited due to its faintness. Using all-sky maps obtained from the Diffuse Infrared Background Experiment, we investigate the scattering property from diffuse Galactic light (DGL) measurements at 1.25, 2.2, and 3.5 μm, in addition to our recent analyses of diffuse near-IR emission. As a result, we first find that the intensity ratios of near-IR DGL to 100 μm emission increase toward low Galactic latitudes at 1.25 and 2.2 μm. The derived latitude dependence can be reproduced by a scattered light model of interstellar dust with a large scattering asymmetry factor g ≡ 'cos θ' of 0.8-0.3+0.2 at 1.25 and 2.2 μm, assuming an infinite Galaxy disk as an illuminating source. The derived asymmetry factor is comparable to the values obtained in the optical, but several times larger than that expected from a recent dust model. Since a possible latitude dependence of ultraviolet-excited dust emission at 1.25 and 2.2 μm would reduce the large asymmetry factor to the reasonable value, our result may indicate the first detection of such an additional emission component in the diffuse interstellar medium.

    DOI: 10.3847/2041-8205/821/1/L11

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84964225040&origin=inward

  • MEASUREMENTS OF DIFFUSE SKY EMISSION COMPONENTS IN HIGH GALACTIC LATITUDES AT 3.5 and 4.9 μm USING DIRBE AND WISE DATA 査読有り

    Sano K., Kawara K., Matsuura S., Kataza H., Arai T., Matsuoka Y.

    Astrophysical Journal   818 ( 1 )   2016年02月

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    担当区分:筆頭著者   記述言語:英語   掲載種別:研究論文(学術雑誌)

    © 2016. The American Astronomical Society. All rights reserved. Using all-sky maps obtained from the Cosmic Background Explorer/Diffuse Infrared Background Experiment (DIRBE) at 3.5 and 4.9 μm, we present a reanalysis of diffuse sky emissions such as zodiacal light (ZL), diffuse Galactic light (DGL), integrated starlight (ISL), and isotropic residual emission including the extragalactic background light (EBL). Our new analysis, which includes an improved estimate of ISL using the Wide-field Infrared Survey Explorer data, enabled us to find the DGL signal in a direct linear correlation between diffuse near-infrared and 100 μm emission at high Galactic latitudes (|b| > 35°). At 3.5 μm, the high-latitude DGL result is comparable to the low-latitude value derived from the previous DIRBE analysis. In comparison with models of the DGL spectrum assuming a size distribution of dust grains composed of amorphous silicate, graphite, and polycyclic aromatic hydrocarbon (PAH), the measured DGL values at 3.5 and 4.9 μm constrain the mass fraction of PAH particles in the total dust species to be more than ∼2%. This was consistent with the results of Spitzer/IRAC toward the lower Galactic latitude regions. The derived residual emission of 8.9 ± 3.4 nWm-2 sr-1 at 3.5 μm is marginally consistent with the level of integrated galaxy light and the EBL constraints from the γ-ray observations. The residual emission at 4.9 μm is not significantly detected due to the large uncertainty in the ZL subtraction, the same as in previous studies. Combined with our reanalysis of the DIRBE data at 1.25 and 2.2 μm, the residual emission in the near-infrared exhibits the Rayleigh-Jeans spectrum.

    DOI: 10.3847/0004-637X/818/1/72

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84959197623&origin=inward

  • DERIVATION of A LARGE ISOTOPIC DIFFUSE SKY EMISSION COMPONENT at 1.25 and 2.2 μm from the COBE/DIRBE DATA 査読有り

    Sano K., Kawara K., Matsuura S., Kataza H., Arai T., Matsuoka Y.

    Astrophysical Journal   811 ( 2 )   2015年10月

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    担当区分:筆頭著者   記述言語:英語   掲載種別:研究論文(学術雑誌)

    � 2015. The American Astronomical Society. All rights reserved. Using all-sky maps obtained with COBE/DIRBE, we reanalyzed the diffuse sky brightness at 1.25 and which consists of zodiacal light, diffuse Galactic light (DGL), integrated starlight (ISL), and isotropic emission including the extragalactic background light. Our new analysis including an improved estimate of the DGL and the ISL with the 2MASS data showed that deviations of the isotropic emission from isotropy were less than 10% in the entire sky at high Galactic latitude (). We derived the DGL to 100 μm brightness ratios of ∼4.79 and ∼1.49 n W m-2 MJy-1 at 1.25 and 2.2 μm, respectively. The result of our analysis revealed a significantly large isotropic component at 1.25 and with intensities of 60.15 16.14 and respectively. This intensity is larger than the integrated galaxy light, upper limits from γ-ray observation, and potential contribution from exotic sources (i.e., Population III stars, intrahalo light, direct collapse black holes, and dark stars). We therefore conclude that the excess light may originate from the local universe: the Milky Way and/or the solar system.

    DOI: 10.1088/0004-637X/811/2/77

    Scopus

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  • Inferred Measurements of the Zodiacal Light Absolute Intensity through Fraunhofer Absorption Line Spectroscopy with CIBER 査読有り 国際誌

    Korngut P.M., Kim M.G., Arai T., Bangale P., Bock J., Cooray A., Cheng Y.T., Feder R., Hristov V., Lanz A., Lee D.H., Levenson L., Matsumoto T., Matsuura S., Nguyen C., Sano K., Tsumura K., Zemcov M.

    Astrophysical Journal   926 ( 2 )   2022年02月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)

    Scattered sunlight from the interplanetary dust (IPD) cloud in our solar system presents a serious foreground challenge for spectrophotometric measurements of the extragalactic background light (EBL). In this work, we report on inferred measurements of the absolute intensity of the zodiacal light (ZL) using the novel technique of Fraunhofer line spectroscopy on the deepest 8542 Å line of the near-infrared Ca ii absorption triplet. The measurements are performed with the narrow band spectrometer (NBS) on board the Cosmic Infrared Background Experiment sounding rocket instrument. We use the NBS data to test the accuracy of two ZL models widely cited in the literature, the Kelsall and Wright models, which have been used in foreground removal analyses that produce high and low EBL results respectively. We find a mean reduced χ 2 = 3.5 for the Kelsall model and χ 2 = 2.0 for the Wright model. The best description of our data is provided by a simple modification to the Kelsall model, which includes a free ZL offset parameter. This adjusted model describes the data with a reduced χ 2 = 1.5 and yields an inferred offset amplitude of 46 ± 19 nW m-2 sr-1 extrapolated to 12500 Å. These measurements elude to the potential existence of a dust cloud component in the inner solar system whose intensity does not strongly modulate with the Earth's motion around the Sun.

    DOI: 10.3847/1538-4357/ac44ff

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85125731172&origin=inward

  • Polarization Spectrum of Near-Infrared Zodiacal Light Observed with CIBER 査読有り 国際誌

    Takimoto K., Arai T., Matsuura S., Bock J.J., Cooray A., Feder R.M., Korngut P.M., Lanz A., Lee D.H., Matsumoto T., Nguyen C.H., Onishi Y., Sano K., Shirahata M., Takahashi A., Tsumura K., Zemcov M.

    Astrophysical Journal   926 ( 1 )   2022年02月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)

    We report the first measurement of the zodiacal light (ZL) polarization spectrum in the near-infrared between 0.8 and 1.8 μm. Using the low-resolution spectrometer on board the Cosmic Infrared Background Experiment, calibrated for absolute spectrophotometry and spectropolarimetry, we acquire long-slit polarization spectral images of the total diffuse sky brightness toward five fields. To extract the ZL spectrum, we subtract the contribution of other diffuse radiation, such as the diffuse galactic light, the integrated starlight, and the extragalactic background light. The measured ZL polarization spectrum shows little wavelength dependence in the near-infrared, and the degree of polarization clearly varies as a function of the ecliptic coordinates and solar elongation. Among the observed fields, the North Ecliptic Pole shows the maximum degree of polarization of ∼20%, which is consistent with an earlier observation from the Diffuse Infrared Background Experiment on board on the Cosmic Background Explorer. The measured degree of polarization and its solar elongation dependence are reproduced by an empirical scattering model in the visible band and also by a Mie scattering model for large absorptive particles, while a Rayleigh scattering model is ruled out. All of our results suggest that the interplanetary dust is dominated by large particles.

    DOI: 10.3847/1538-4357/ac416f

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85125862787&origin=inward

  • Probing Intra-Halo Light with Galaxy Stacking in CIBER Images 査読有り 国際誌

    Yun-Ting Cheng, Toshiaki Arai, Priyadarshini Bangale, James J. Bock, Tzu-Ching Chang, Asantha Cooray, Richard M. Feder, Phillip M. Korngut, Dae Hee Lee, Lunjun Liu, Toshio Matsumoto, Shuji Matsuura, Chi H. Nguyen, Kei Sano, Kohji Tsumura, Michael Zemcov

    THE ASTROPHYSICAL JOURNAL   919 ( 2 )   69   2021年10月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)

    We study the stellar halos of 0.2 ≲ z ≲ 0.5 galaxies with stellar masses spanning M ∗ ∼ 1010.5 to 1012 M o˙ (approximately L ∗ galaxies at this redshift) using imaging data from the Cosmic Infrared Background Experiment (CIBER). A previous CIBER fluctuation analysis suggested that intra-halo light (IHL) contributes a significant portion of the near-infrared extragalactic background light (EBL), the integrated emission from all sources throughout cosmic history. In this work, we carry out a stacking analysis with a sample of ∼30,000 Sloan Digital Sky Survey (SDSS) photometric galaxies from CIBER images in two near-infrared bands (1.1 and 1.8 μm) to directly probe the IHL associated with these galaxies. We stack galaxies in five sub-samples split by brightness and detect an extended galaxy profile beyond the instrument point-spread function (PSF) derived by stacking stars. We jointly fit a model for the inherent galaxy light profile plus large-scale one- and two-halo clustering to measure the extended galaxy IHL. We detect nonlinear one-halo clustering in the 1.8 μm band at a level consistent with numerical simulations. By extrapolating the fraction of extended galaxy light we measure to all galaxy mass scales, we find ∼30%/15% of the total galaxy light budget from galaxies is at radius r > 10/20 kpc, respectively. These results are new at near-infrared wavelengths at the L ∗ mass scale and suggest that the IHL emission and one-halo clustering could have appreciable contributions to the amplitude of large-scale EBL background fluctuations.

    DOI: 10.3847/1538-4357/ac0f5b

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85116880861&origin=inward

  • Development of an optical and near-infrared telescope onboard the HiZ-GUNDAM mission 査読有り 国際誌

    Tsumura K., Yonetoku D., Kawabata K., Matsuura S., Noda H., Urata Y., Niino Y., Sano K., Ohashi A., Doi A., Akitaya H., Miyasaka A., Kurimata M., Kawata Y., Arimoto M., Okita H.

    Proceedings of SPIE - The International Society for Optical Engineering   11443   2020年12月

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    記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    © COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only. The HiZ-GUNDAM (high-z Gamma-ray bursts for UNraveling the Dark Ages Mission) is a time-domain and multi-messenger astronomy mission by monitoring high-energy astronomical transient events such as gamma-ray bursts (GRBs). The HiZ-GUNDAM is designed to provide alerts of high-redshift GRBs with an ultra-wide field X-ray monitor and a co-onboard 30-cm telescope for immediate photometric follow-up observations in the visible and near-infrared. The HiZ-GUNDAM satellite automatically changes its attitude toward the discovered transient object, starts the follow-up observations with the telescope, and sends alert information including the detailed position, the apparent magnitude and photometric redshift of the transient object within one hour. This mission was selected as one of the mission concept candidates of the competitively-chosen medium-class mission of ISAS/JAXA in the mid-2020s. The basic design of the breadboard model of the telescope is undergoing, and the verification plan of it is studied. The optics are cooled down to 200 K by radiation cooling, and infrared detectors are additionally cooled down to 120 K by a mechanical cooler. All mirrors in the telescope are made of the same aluminum-alloy to reduce the alignment errors during cooling. The four-band simultaneous observation is realized by three beam splitters. The HgCdTe and HyViSi detectors are installed in this telescope. Basic technologies for these specifications are demonstrated by our other missions. In addition, the onboard detection algorithm of high-redshift GRBs by distinguishing them from nearby dusty galaxies in the orbit is also studied. In this paper, we introduce the current status of the development of the telescope onboard HiZ-GUNDAM.

    DOI: 10.1117/12.2560654

    Scopus

    その他リンク: https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85099292690&origin=inward

  • Development of EXo-Zodiacal Infrared Telescope (EXZIT) for observation of visible and near-infrared extragalactic background light 査読有り 国際誌

    Sano K., Matsuura S., Tsumura K., Takahashi A., Hashimoto R., Ogura S., Yomo K., Yasutake H., Ino Y., Tanaka R.

    Proceedings of SPIE - The International Society for Optical Engineering   11443   2020年12月

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    担当区分:筆頭著者   記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    © COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only. Extragalactic background light (EBL) consists of entire radiation emitted throughout the cosmic history and is one crucial observable quantity to study astrophysics in the early universe, such as first stellar objects or primordial black holes. In the visible and near-infrared, zodiacal light (ZL), sunlight scattered by interplanetary dust, is the brightest foreground for observer in the near-earth orbit and its uncertainty limits accuracy of the EBL measurement. To overcome this problem, observations from heliocentric distance beyond 5 au, where the ZL is negligible, is promising. To achieve the EBL observation in deep space, we have been developing EXo- Zodiacal Infrared Telescope (EXZIT) onboard a solar sail spacecraft to Jovian Trojans planned in Japan around 2030. According to our mission study, a three-mirror reflective telescope optics design with a 90mm × 50mm effective aperture and 16 deg × 8 deg field of view (FoV) followed by a focal plane array HAWAII-2RG with a linear variable filter makes available to detect the EBL at high significance in 0.4-1.6 μm with specific wavelength resolution of ∼20. In the present study, we develop test optics to demonstrate optical performance in room temperature for the future observation. By adopting only mirrors of aspherical surface, we design the optics whose aberration is minimized to show point spread function (PSF) of approximately 3 pix × 3 pix on the focal plane. The mirrors are fabricated by machining aluminum alloy A6061 with a honeycomb processing on the back surface to reduce the mirror mass. After integrating and aligning the mirrors with support jigs, we measure the PSF on the focal plane by a visible camera by inserting collimated beam of different angle of incidence, covering the whole FoV. We evaluate the PSF size by analyzing encircled energy in comparison with that expected from the ray-trace simulation of the optics. Throughout the FoV of the optics, the measured PSF size is comparable to the simulation. The present study demonstrates the precision machining of the aspherical mirrors and the optical performance of the designed optics. As a next step, we plan to develop thermal structure of EXZIT to demonstrate the optical performance in low temperature.

    DOI: 10.1117/12.2559169

    Scopus

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  • Pre-flight optical test and calibration for the Cosmic Infrared Background ExpeRiment 2 (CIBER-2) 査読有り 国際誌

    Takimoto K., Bang S.C., Bangale P., Bock J.J., Cooray A., Danbayashi K., Feder R.M., Furutani M., Gates K., Hashimoto R., Hristov V., Kida A., Korngut P., Lanz A., Lee D.H., Liu L., Mason P., Matsumoto T., Matsuura S., Morgan J.A., Nguyen C.H., Park W.K., Patru D., Parkus J., Sakai S., Sano K., Suzuki H., Takahashi A., Tatsu S., Tsumura K., Wada T., Wang S.Y., Yamada Y., Zemcov M.

    Proceedings of SPIE - The International Society for Optical Engineering   11443   2020年12月

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    記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    © COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only. The total integrated emission from galaxies, known as the Extragalactic Background Light (EBL), is an important observable for understanding the history of star formation over the history of the universe. Spatial fluctuations in the infrared EBL as measured by the Cosmic Infrared Background ExpeRiment (CIBER), Spitzer and AKARI exceed the predicted signal from galaxy clustering alone. The CIBER-2 project seeks to extend CIBER observa- tions of the EBL throughout the near infrared into the optical, through measurements above Earth's atmosphere during a suborbital sounding rocket flight. The experiment has a LN2-cooled 28.5 cm Cassegrain telescope along with three optical paths and dichroic beamsplitters, which are used to obtain three wide-field images in six broad spectral bands between 0.5-2.0 μm. The three focal planes also contain linear variable filters (LVFs) which simultaneously take spectra with resolution R=20 across the same range. CIBER-2 is scheduled to y multiple times on a Black Brant IX sounding rocket from White Sands Missile Range in the New Mexico desert. For the first flight, scheduled for early 2021, we have completed a variety of pre-flight optical tests, which we use to make focus adjustments, spectral response measurements, and absolute photometric calibrations. In this paper, we describe the methods behind these tests and present their results for pre-flight performance evaluation. In particular, we present measurements of the PSF for each broad spectral band, along with absolute calibration factors for each band and the LVF. Through monochromator scans, we also measure the spectral responsivity of each LVF as a function of position.

    DOI: 10.1117/12.2561917

    Scopus

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  • High-redshift gamma-ray burst for unraveling the Dark Ages Mission - HiZ-GUNDAM - 国際誌

    Yonetoku D., Mihara T., Doi A., Sakamoto T., Tsumura K., Ioka K., Amaya Y., Arimoto M., Enoto T., Fujii T., Goto H., Gunji S., Hiraga J., Ikeda H., Kawai N., Kurosawa S., Li J., Maeda Y., Mitsuishi I., Murakami T., Nakagawa Y., Ogino N., Ohno M., Sawano T., Sei K., Serino M., Sugita S., Tamagawa T., Tamura K., Tanaka T., Tanimori T., Tashiro M.S., Tomida H., Wang H., Yamaguchi T., Yamamoto A., Yamaoka K., Yamauchi M., Yatsu Y., Yoshida A., Yuhi D., Akitaya H., Fukui A., Ita Y., Kaneda H., Kawabata K., Kawata Y., Kurimata M., Matsumoto T., Matsuura S., Miyasaka A., Motohara K., Narita N., Noda H., Ohashi A., Okita H., Sano K., Tanaka M., Urata Y., Wada T., Yamaguchi H., Yanagisawa K., Yoshida M., Asano K., Inayoshi K., Inoue S., Ito H., Izumiura H., Kawanaka N., Kinugawa T., Kisaka S., Kiuchi K., Kyutoku K., Matsumoto J., Mizuta A., Murase K., Nagakura H., Nagataki S., Nakada Y., Nakamura T., Niino Y., Suwa Y., Takahashi K., Tanaka T., Toma K., Totani T., Yamazaki R., Yokoyama J.

    Proceedings of SPIE - The International Society for Optical Engineering   11444   2020年12月

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    担当区分:責任著者   記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    HiZ-GUNDAM is a future satellite mission which will lead the time-domain astronomy and the multi-messenger astronomy through observations of high-energy transient phenomena. A mission concept of HiZ-GUNDAM was approved by ISAS/JAXA, and it is one of the future satellite candidates of JAXA's medium-class mission. We are in pre-phase A (before pre-project) and elaborating the mission concept, mission/system requirements for the launch in the late 2020s. The main themes of HiZ-GUNDAM mission are (1) exploration of the early universe with high-redshift gamma-ray bursts, and (2) contribution to the multi-messenger astronomy. HiZ-GUNDAM has two kinds of mission payload. The wide field X-ray monitors consist of Lobster Eye optics array and focal imaging sensor, and monitor ~1 steradian field of view in 0.5 - 4 keV energy range. The near infrared telescope has an aperture size 30 cm in diameter, and simultaneously observes four wavelength bands between 0.5 - 2.5 µm. In this paper, we introduce the mission overview of HiZ-GUNDAM.

    DOI: 10.1117/12.2560603

    Scopus

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  • MIRIS observation of near-infrared diffuse Galactic light 査読有り

    Onishi Y., Sano K., Matsuura S., Jeong W.S., Pyo J., Kim I.J., Seo H.J., Han W., Lee D.H., Moon B., Park W., Park Y., Kim M.G., Matsumoto T., Matsuhara H., Nakagawa T., Tsumura K., Shirahata M., Arai T., Ienaka N.

    Publications of the Astronomical Society of Japan   70 ( 4 )   2018年08月

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    担当区分:責任著者   記述言語:英語   掲載種別:研究論文(学術雑誌)

    © The Author(s) 2018. Published by Oxford University Press on behalf of the Astronomical Society of Japan. All rights reserved. We report near-infrared (IR) observations of high Galactic latitude clouds to investigate diffuse Galactic light (DGL), which is starlight scattered by interstellar dust grains. The observations were performed at 1.1 and 1.6 μm with a wide-field camera instrument, the Multi-purpose Infra-Red Imaging System (MIRIS) onboard the Korean satellite STSAT-3. The DGL brightness is measured by correlating the near-IR images with a far-IR 100 μm map of interstellar dust thermal emission. The wide-field observation of DGL provides the most accurate DGL measurement achieved to-date. We also find a linear correlation between optical and near-IR DGL in the MBM32 field. To study interstellar dust properties in MBM32, we adopt recent dust models with and without μm-sized very large grains and predict the DGL spectra, taking into account the reddening effect of the interstellar radiation field. The result shows that the observed color of the near-IR DGL is closer to the model spectra without very large grains. This may imply that dust growth in the observed MBM32 field is not active owing to the low density of its interstellar medium.

    DOI: 10.1093/pasj/psy070

    Scopus

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  • Integration and instrument characterization of the cosmic infrared background experiment 2 (CIBER-2) 査読有り

    Nguyen C., Stewart B., Bang S., Bock J., Cooray A., Danbayashi K., Desantiago A., Hristov V., Kojima T., Korngut P., Kruse K., Lanz A., Lee D., Liu L., Loewenthal J., Mason P., Matsumoto T., Matsuura S., Ohta R., Pape C., Park W., Patru D., Parkus J., Sano K., Takahashi A., Peryer M., Takimoto K., Tsumura K., Wada T., Wang S., Yamada Y., Zemcov M.

    Proceedings of SPIE - The International Society for Optical Engineering   10698   2018年01月

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    記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    © COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only. The extragalactic background light (EBL) is the integrated emission from all objects outside of the Milky Way galaxy. Imprinted by the history of stellar emission, the EBL in the near infrared traces light back to the birth of the first stars in the Universe and can allow tight constraints on structure formation models. Recent studies using data from the Spitzer Space Telescope and the first Cosmic Infrared Background ExpeRiment (CIBER-1) find that there are excess fluctuations in the EBL on large scales which have been attributed to either high redshift galaxies and quasars, or to stars that were stripped from their host galaxies during merging events. To help disentangle these two models, multi-wavelength data can be used to trace their distinctive spectral features. Following the success of CIBER-1, CIBER-2 is designed to identify the sources of the EBL excess fluctuations using data in six wavebands covering the optical and near infrared. The experiment consists of a cryogenic payload and is scheduled to launch four times on a recoverable sounding rocket. CIBER-2 has a 28.5 cm telescope coupled with an optics system to obtain wide-field images in six broad spectral bands between 0.5 and 2.5 μm simultaneously. The experiment uses 2048 × 2048 Hawaii-2RG detector arrays and a cryogenic star tracker. A prototype of the cryogenic star tracker is under construction for a separate launch to verify its performance and star tracking algorithm. The mechanical, optical, and electrical components of the CIBER-2 experiment will have been integrated into the payload by mid-2018. Here we present the final design of CIBER-2 and our team's instrument characterization efforts. The design and analysis of the optical focus tests will be discussed. We also report on the performance of CIBER-2 support systems, including the cooling mechanisms and deployable components. Finally, we outline the remaining tasks required to prepare the payload for launch.

    DOI: 10.1117/12.2311595

    Scopus

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  • Development of data storage system and GSE for cosmic infrared background experiment 2 (CIBER-2) 査読有り

    Park W.K., Bang S.C., Battle J., Bock J., Cooray A., Danbayashi K., Desantiago A., Hristov V., Kojima T., Korngut P., Lanz A., Lee D.H., Liu L., Loewenthal J., Mason P., Matsumoto T., Matsuura S., Nguyen C.H., Ohta R., Patru D., Peyer M., Sano K., Takahashi A., Takimoto K., Tsumura K., Wada T., Wang S.Y., Yamada Y., Zemcov M.

    Proceedings of SPIE - The International Society for Optical Engineering   10698   2018年01月

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    記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    © COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only. Cosmic Infrared Background ExpeRiment-2 (CIBER-2) is an international project to make a rocket-borne measurement of the Cosmic Infrared Background (CIB) using three Hawaii-2RG image sensors. Since the rocket telemetry is unable to downlink all the image data in real time, we adopt an onboard data storage board for each sensor electronics. In this presentation, the development of the data storage board and the Ground Station Electronics (GSE) system for CIBER2 are described. We have fabricated, integrated, and tested all systems and confirmed that all work as expected, and are ready for flight.

    DOI: 10.1117/12.2313184

    Scopus

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  • Ultraviolet to optical diffuse sky emission as seen by the Hubble Space Telescope Faint Object Spectrograph 査読有り

    Kawara K., Matsuoka Y., Sano K., Brandt T., Sameshima H., Tsumura K., Oyabu S., Ienaka N.

    Publications of the Astronomical Society of Japan   69 ( 2 )   2017年01月

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    担当区分:責任著者   記述言語:英語   掲載種別:研究論文(学術雑誌)

    © The Author 2017. Published by Oxford University Press on behalf of the Astronomical Society of Japan. All rights reserved. We present an analysis of the blank-sky spectra observed with the Faint Object Spectrograph on board the Hubble Space Telescope. We study the diffuse sky emission from ultraviolet to optical wavelengths, which is composed of zodiacal light (ZL), diffuse Galactic light (DGL), and residual emission. The observations were performed towards 54 fields distributed widely over the sky, with spectral coverage from 0.2 to 0.7 μm. In order to avoid contaminating light from earthshine, we use the data collected only in orbital nighttime. The observed intensity is decomposed into the ZL, DGL, and residual emission, in eight photometric bands spanning our spectral coverage. We found that the derived ZL reflectance spectrum is flat in the optical, which indicates major contribution of C-type asteroids to the interplanetary dust (IPD). In addition, the ZL reflectance spectrum has an absorption feature at ∼0.3 μm. The shape of the DGL spectrum is consistent with those found in earlier measurements and model predictions. While the residual emission contains a contribution from the extragalactic background light, we found that the spectral shape of the residual looks similar to the ZL spectrum. Moreover, its optical intensity is much higher than that measured from beyond the IPD cloud by Pioneer 10/11, and also than that of the integrated galaxy light. These findings may indicate the presence of an isotropic ZL component, which is missed in the conventional ZL models.

    DOI: 10.1093/pasj/psx003

    Scopus

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  • The cosmic infrared background experiment-2 (CIBER-2) for studying the near-infrared extragalactic background light 査読有り

    Shirahata M., Arai T., Battle J., Bock J., Cooray A., Enokuchi A., Hristov V., Kanai Y., Kim M.G., Korngut P., Lanz A., Lee D.H., Mason P., Matsumoto T., Matsuura S., Morford T., Ohnishi Y., Park W.K., Sano K., Takeyama N., Tsumura K., Wada T., Wang S.Y., Zemcov M.

    Proceedings of SPIE - The International Society for Optical Engineering   9904   2016年01月

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    記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)

    © 2016 SPIE. We present the current status of the Cosmic Infrared Background ExpeRiment-2 (CIBER-2) project, whose goal is to make a rocket-borne measurement of the near-infrared Extragalactic Background Light (EBL), under a collaboration with U.S.A., Japan, South Korea, and Taiwan. The EBL is the integrated light of all extragalactic sources of emission back to the early Universe. At near-infrared wavelengths, measurement of the EBL is a promising way to detect the diffuse light from the first collapsed structures at redshift zâ1/410, which are impossible to detect as individual sources. However, recently, the intra-halo light (IHL) model is advocated as the main contribution to the EBL, and our new result of the EBL fluctuation from CIBER-1 experiment is also supporting this model. In this model, EBL is contributed by accumulated light from stars in the dark halo regions of low- redshift (z<2) galaxies, those were tidally stripped by the interaction of satellite dwarf galaxies. Thus, in order to understand the origin of the EBL, both the spatial fluctuation observations with multiple wavelength bands and the absolute spectroscopic observations for the EBL are highly required. After the successful initial CIBER- 1 experiment, we are now developing a new instrument CIBER-2, which is comprised of a 28.5-cm aluminum telescope and three broad-band, wide-field imaging cameras. The three wide-field (2.3×2.3 degrees) imaging cameras use the 2K×2K HgCdTe HAWAII-2RG arrays, and cover the optical and near-infrared wavelength range of 0.5-0.9 μm, 1.0-1.4 μm and 1.5-2.0 μm, respectively. Combining a large area telescope with the high sensitivity detectors, CIBER-2 will be able to measure the spatial fluctuations in the EBL at much fainter levels than those detected in previous CIBER-1 experiment. Additionally, we will use a linear variable filter installed just above the detectors so that a measurement of the absolute spectrum of the EBL is also possible. In this paper, the scientific motivation and the expected performance for CIBER-2 will be presented. The detailed designs of the telescope and imaging cameras will also be discussed, including the designs of the mechanical, cryogenic, and electrical systems.

    DOI: 10.1117/12.2229567

    Scopus

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  • MEASUREMENTS of the MEAN DIFFUSE GALACTIC LIGHT SPECTRUM in the 0.95-1.65 μm BAND from CIBER 査読有り

    Arai T., Matsuura S., Bock J., Cooray A., Kim M., Lanz A., Lee D., Lee H., Sano K., Smidt J., Matsumoto T., Nakagawa T., Onishi Y., Korngut P., Shirahata M., Tsumura K., Zemcov M.

    Astrophysical Journal   806 ( 1 )   2015年06月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)

    © 2015. The American Astronomical Society. All rights reserved. We report measurements of the diffuse galactic light (DGL) spectrum in the near-infrared, spanning the wavelength range 0.95-1.65 μm by the Cosmic Infrared Background ExpeRiment. Using the low-resolution spectrometer calibrated for absolute spectro-photometry, we acquired long-slit spectral images of the total diffuse sky brightness toward six high-latitude fields spread over four sounding rocket flights. To separate the DGL spectrum from the total sky brightness, we correlated the spectral images with a 100 μm intensity map, which traces the dust column density in optically thin regions. The measured DGL spectrum shows no resolved features and is consistent with other DGL measurements in the optical and at near-infrared wavelengths longer than 1.8 μm. Our result implies that the continuum is consistently reproduced by models of scattered starlight in the Rayleigh scattering regime with a few large grains.

    DOI: 10.1088/0004-637X/806/1/69

    Scopus

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口頭発表・ポスター発表等

  • 光赤外線波長における天文観測と宇宙天気 招待有り

    佐野圭

    第150回 地球電磁気・地球惑星圏学会 総会・講演会および一般公開イベント 

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    開催期間: 2021年11月01日 - 2021年11月04日   記述言語:日本語   開催地:オンライン  

  • 超小型衛星による宇宙可視光背景放射観測ミッション

    佐野圭(九州工業大学),中川貴雄,松原英雄,磯部直樹,宮﨑康行(JAXA),松浦周二(関西学院大学),津村耕司(東京都市大学)

    超小型衛星利用シンポジウム2022 

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    開催期間: 2022年01月18日   記述言語:日本語   開催地:X-NIHONBASHI TOWER  

    我々は、超小型衛星による宇宙可視光背景放射観測ミッションの検討を進めている。宇宙背景放射は、宇宙初期から現在までに放射された光の総計であり、宇宙の星形成史を解明するための重要な観測量である。等方な強さを持つ宇宙背景放射の観測は高い解像度や指向精度を必要としないため、6Uサイズの超小型衛星に比較的小口径の望遠鏡を搭載することで実現可能なミッションである。

  • 可視近赤外宇宙背景放射観測装置EXZIT:金属鏡表面粗さの評価

    佐野圭、橋本遼、松浦周二、猪裕太、松見知香、石田魁、林広憲、津村耕司

    日本天文学会2021年秋季年会 

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    開催期間: 2021年09月13日 - 2021年09月15日   記述言語:日本語  

  • 金属蒸着アルミニウム鏡の異種金属接触腐食による反射率低下現象の検証

    佐野圭 他

    日本天文学会2021年春季年会 

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    開催期間: 2021年03月   記述言語:日本語  

  • 深宇宙における宇宙背景放射観測に向けた可視光近赤外線望遠鏡の開発

    佐野圭, 松浦周二, 橋本遼, 小倉颯太, 安竹彦馬, 猪裕太, 田中怜奈, 津村耕司

    日本天文学会2021年春季年会 

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    開催期間: 2021年03月   記述言語:日本語  

  • New measurement of the near-infrared extragalactic background light by evaluation of isotropic interplanetary dust

    Kei Sano, Shuji Matsuura, Kazuma Yomo, Aoi Takahashi

    GALAXY EVOLUTION WORKSHOP 2020 

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    開催期間: 2021年02月02日 - 2021年02月05日   記述言語:英語  

  • Development of EXo-Zodiacal Infrared Telescope (EXZIT) for observation of visible and near-infrared extragalactic background light

    Sano K., Matsuura S., Tsumura K., Takahashi A., Hashimoto R., Ogura S., Yomo K., Yasutake H., Ino Y., Tanaka R.

    SPIE Astronomical Telescopes + Instrumentation Digital Forum  

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    開催期間: 2020年12月   記述言語:英語  

  • 宇宙赤外線背景放射観測実験CIBER-2の進捗状況

    佐野圭 他

    第2回観測ロケットシンポジウム 

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    開催期間: 2019年08月   記述言語:日本語  

  • Spectral Study of Scattered Light by Interstellar Dust Grains

    Kei Sano

    IAU Symposium PanModel2018:Challenges in Panchromatic Galaxy Modeling with Next Generation Facilities 

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    開催期間: 2018年11月   記述言語:英語  

  • Measurement of Infrared Extragalactic Background Light Considering Interplanetary Dust Particles from Oort-cloud Comets

    Sano, K., Matsuura, S., Takahashi, A.

    Cosmic DUST XI 

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    開催期間: 2018年08月   記述言語:英語  

  • Size Distribution of Interstellar Dust Constrained by Near-infrared Diffuse Galactic Light Observed with MIRIS

    Sano, K. 他

    Cosmic DUST XI 

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    開催期間: 2018年08月   記述言語:英語  

  • Separation of the Near-Infrared Extragalactic Background Light and Scattered Sunlight by Interplanetary Dust

    Sano, K., Matsuura, S., Takahashi, A.

    Cosmic DUST X 

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    開催期間: 2017年08月   記述言語:英語  

  • Interstellar Dust Properties Revealed by Diffuse Galactic Light Measurements

    Sano, K. 他

    Workshop on interstellar Matter 2016 

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    開催期間: 2016年10月   記述言語:英語  

  • Measurement of Near-Infrared Diffuse Galactic Light

    Sano, K. 他

    Cosmic DUST IX 

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    開催期間: 2016年08月   記述言語:英語  

▼全件表示

報道関係

  • 九工大とマレーシアプトラ大 オンラインモビリティプログラム   会誌・広報誌

    九州工業大学

    文教ニュース社  文教ニュース  2021年07月19日

  • 九工大、UPMとEモビリティプログラム   会誌・広報誌

    九州工業大学

    官庁通信社  文教速報  2021年07月19日

  • 宇宙最初の星探し、宇宙赤外線背景放射をロケットで観測   インターネットメディア

    松浦周二(関西学院大学),佐野圭(九州工業大学),津村耕司(東京都市大学)

    AstroArts  2021年06月11日

科研費獲得実績

  • 近赤外線域における宇宙背景放射と銀河拡散光の研究

    研究課題番号:26・7628  2014年04月 - 2017年03月   特別研究員奨励費

その他競争的資金獲得実績

  • 可視光赤外線における宇宙観測用望遠鏡のコート方法の探求

    2022年04月 - 2023年03月

    ISAS/JAXA 大学共同利用(宇宙放射線)  

  • 可視光赤外線における宇宙観測用望遠鏡のコート方法の探求

    2021年04月 - 2022年03月

    ISAS/JAXA 大学共同利用(宇宙放射線)  

  • 可視光赤外線における宇宙観測用望遠鏡のコート方法の探求

    2020年04月 - 2021年03月

    ISAS/JAXA 大学共同利用(宇宙放射線)  

海外研究歴

  • 観測ロケット実験CIBER-2の開発

    カリフォルニア工科大学、ワロップス飛行施設  アメリカ合衆国  研究期間:  2019年05月 - 2019年07月

  • 観測ロケット実験CIBER-2の開発

    カリフォルニア工科大学  アメリカ合衆国  研究期間:  2019年01月 - 2019年03月

  • 観測ロケット実験CIBER-2の開発

    カリフォルニア工科大学  アメリカ合衆国  研究期間:  2018年10月 - 2018年12月

  • 観測ロケット実験CIBER-2の開発

    カリフォルニア工科大学  アメリカ合衆国  研究期間:  2018年05月 - 2018年07月

  • 観測ロケット実験CIBER-2の開発

    カリフォルニア工科大学  アメリカ合衆国  研究期間:  2018年01月 - 2018年03月

担当授業科目(学内)

  • 2021年度   宇宙システム工学入門

学会・委員会等活動

  • 日本天文学会 キャリア支援委員会   委員  

    2021年06月 - 2023年05月

PR

  • (学生向けPR)

    光赤外線天文学に関する研究を行っています。ロケットや衛星に搭載する観測装置や天文観測データの解析を行っています。