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33 results on '"Chiyonobu, S."'

1. Site U1599.

Author

Druitt, T. H., Kutterolf, S., Ronge, T. A., Beethe, S., Bernard, A., Berthod, C., Chen, H., Chiyonobu, S., Clark, A., DeBari, S., Fernandez Perez, T. I., Gertisser, R., Hübscher, C., Johnston, R. M., Jones, C., Joshi, K. B., Kletetschka, G., Koukousioura, O., Li, X., and Manga, M.

Subjects
OCEAN, VOLCANIC ash, tuff, etc., CLASTIC rocks, BIOSPHERE, PLANETS
Published
2024
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2. Site U1600.

Author

Kutterolf, S., Druitt, T. H., Ronge, T. A., Beethe, S., Bernard, A., Berthod, C., Chen, H., Chiyonobu, S., Clark, A., DeBari, S., Fernandez Perez, T. I., Gertisser, R., Hübscher, C., Johnston, R. M., Jones, C., Joshi, K. B., Kletetschka, G., Koukousioura, O., Li, X., and Manga, M.

Subjects
CLASTIC rocks, BIOSPHERE
Published
2024
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3. Expedition 398 summary.

Author

Druitt, T. H., Kutterolf, S., Ronge, T. A., Beethe, S., Bernard, A., Berthod, C., Chen, H., Chiyonobu, S., Clark, A., DeBari, S., Fernandez Perez, T. I., Gertisser, R., Hübscher, C., Johnston, R. M., Jones, C., Joshi, K. B., Kletetschka, G., Koukousioura, O., X. Li, and Manga, M.

Subjects
OCEAN, DRILLING platforms, VOLCANOLOGY, BIOSTRATIGRAPHY, PALEOBIOLOGY
Abstract

The objectives of International Ocean Discovery Program Expedition 398, Hellenic Arc Volcanic Field (11 December 2022 to 10 February 2023), were to study the volcanic record of the central Hellenic island arc; document the links and feedbacks between volcanism/magmatism, crustal tectonics, and sea level; investigate the processes and products of shallow submarine eruptions of silicic magma; and groundtruth the seismic stratigraphy of Santorini caldera. Reconstructing the subsidence history of the southern Aegean Sea and searching for deep life inside and outside of Santorini caldera were additional objectives. During the expedition, 10 primary and alternate sites that were originally proposed were drilled, in addition to 2 extra sites that were requested during the expedition. Outside of Santorini caldera, drilling penetrated the thick basin fills of the crustal rift system hosting the Christiana-Santorini- Kolumbo volcanic field, identifying numerous pumice and ash layers, some known from on land and others hitherto unknown, pushing back the onset of volcanism in the area into the Early Pleistocene or even Pliocene. Significant events of mass wasting into the basins, accompanied by very high sedimentation rates, were also documented. These basin sites served to groundtruth the seismic stratigraphy of the basins and open the way to unraveling relationships between volcanic activity and crustal rift pulses. Two sites of condensed sequences served to sample many volcanic layers within the detailed age-depth constraints provided mainly by biostratigraphy, as diagenetic effects complicated the magnetic reversal record significantly. Drilling penetrated the Alpine basement at three basin sites northeast of Santorini, whereas in the Christiana Basin to the southwest it penetrated a thick sequence of Messinian evaporites. Drilling inside Santorini caldera penetrated to ~120 meters below seafloor, less than planned due to hole instability issues but deep enough to groundtruth the seismic stratigraphy and sample the different layers. One intracaldera hole yielded a detailed tephra record of the history of the Kameni Islands, as well as possible evidence for deep bacterial colonies within the caldera. Despite variable recovery in the unstable pumice and ash deposits, the expedition was a significant success that may address almost all the scientific objectives once the laboratory work has been done. [ABSTRACT FROM AUTHOR]

Published
2024
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4. Expedition 398 methods.

Author

Kutterolf, S., Druitt, T. H., Ronge, T. A., Beethe, S., Bernard, A., Berthod, C., Chen, H., Chiyonobu, S., Clark, A., DeBari, S., Fernandez Perez, T. I., Gertisser, R., Hübscher, C., Johnston, R. M., Jones, C., Joshi, K. B., Kletetschka, G., Koukousioura, O., Li, X., and Manga, M.

Subjects
OCEAN, VOLCANISM, GEODYNAMICS, MARINE ecology
Published
2024
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6. Optical and Near-Infrared Polarimetry of Highly Reddened Type Ia Supernova 2014J: Peculiar Properties of Dust in M82

Author

Kawabata, K. S., Akitaya, H., Yamanaka, M., Itoh, R., Maeda, K., Moritani, Y., Ui, T., Kawabata, M., Mori, K., Nogami, D., Nomoto, K., Suzuki, N., Takaki, K., Tanaka, M., Ueno, I., Chiyonobu, S., Harao, T., Matsui, R., Miyamoto, H., Nagae, O., Nakashima, A., Nakaya, H., Ohashi, Y., Ohsugi, T., Komatsu, T., Sakimoto, K., Sasada, M., Sato, H., Tanaka, H., Urano, T., Yamashita, T., Yoshida, M., Arai, A., Ebisuda, N., Fukazawa, Y., Fukui, A., Hashimoto, O., Honda, S., Izumiura, H., Kanda, Y., Kawaguchi, K., Kawai, N., Kuroda, D., Masumoto, K., Matsumoto, K., Nakaoka, T., Takata, K., Uemura, M., and Yanagisawa, K.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We presented optical and near-infrared multi-band linear polarimetry of the highly reddened Type Ia SN~2014J appeared in M82. SN~2014J exhibits large polarization at shorter wavelengths, e.g., $4.8$\% in $B$ band, and the polarization decreases rapidly at longer wavelengths, with the position angle of the polarization remaining at approximately $40^{\circ}$ over the observed wavelength range. These polarimetric properties suggest that the observed polarization is likely to be caused predominantly by the interstellar dust within M82. Further analysis shows that the polarization peaks at a wavelengths much shorter than those obtained for the Galactic dust. The wavelength dependence of the polarization can be better described by an inverse power law rather than by Serkowski law for Galactic interstellar polarization. These suggests that the nature of the dust in M82 may be different from that in our Galaxy, with polarizing dust grains having a mean radius of $<0.1\ \mu$m., Comment: 8 pages, 4 figures, accepted for publication in ApJ Letters

Published
2014
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7. GRB 091208B: First Detection of the Optical Polarization in Early Forward Shock Emission of a Gamma-Ray Burst Afterglow

Author

Uehara, T., Toma, K., Kawabata, K. S., Chiyonobu, S., Fukazawa, Y., Ikejiri, Y., Inoue, T., Itoh, R., Komatsu, T., Miyamoto, H., Mizuno, T., Nagae, O., Nakaya, H., Ohsugi, T., Sakimoto, K., Sasada, M., Tanaka, H., Uemura, M., Yamanaka, M., Yamashita, T., Yamazaki, R., and Yoshida, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report that the optical polarization in the afterglow of GRB 091208B is measured at t = 149 - 706 s after the burst trigger, and the polarization degree is P = 10.4% +/- 2.5%. The optical light curve at this time shows a power-law decay with index -0.75 +/- 0.02, which is interpreted as the forward shock synchrotron emission, and thus this is the first detection of the early-time optical polarization in the forward shock (rather than that in the reverse shock reported by Steele et al. (2009). This detection disfavors the afterglow model in which the magnetic fields in the emission region are random on the plasma skin depth scales, such as amplified by the plasma instabilities, e.g., Weibel instability. We suggest that the fields are amplified by the magnetohydrodynamic instabilities, which would be tested by future observations of the temporal changes of the polarization degrees and angles for other bursts., Comment: 12 pages, 4 figures, accepted for publication in ApJ Letters

Published
2012
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8. Early phase observations of extremely luminous Type Ia Supernova 2009dc

Author

Yamanaka, M., Kawabata, K. S., Kinugasa, K., Tanaka, M., Imada, A., Maeda, K., Nomoto, K., Arai, A., Chiyonobu, S., Fukazawa, Y., Hashimoto, O., Honda, S., Ikejiri, Y., Itoh, R., Kamata, Y., Kawai, N., Komatsu, T., Kuroda, D., Miyamoto, H., Miyazaki, S., Nagae, O., Nakaya, H., Ohsugi, T., Omodaka, T., Sakai, N., Sasada, M., Suzuki, M., Taguchi, H., Takahashi, H., Tanaka, H., Uemura, M., Yamashita, T., Yanagisawa, K., and Yoshida, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present early phase observations in optical and near-infrared wavelengths for the extremely luminous Type Ia supernova (SN Ia) 2009dc. The decline rate of the light curve is $\Delta m_{15}(B)=0.65\pm 0.03$, which is one of the slowest among SNe Ia. The peak $V$-band absolute magnitude is $M_{V}=-19.90\pm 0.15$ mag even if the host extinction is $A_{V}=0$ mag. It reaches $M_{V}=-20.19\pm 0.19$ mag for the host extinction of $A_{V}=0.29$ mag as inferred from the observed Na {\sc i} D line absorption in the host. Our $JHK_{s}$-band photometry shows that the SN is one of the most luminous SNe Ia also in near-infrared wavelengths. These results indicate that SN 2009dc belongs to the most luminous class of SNe Ia, like SN 2003fg and SN 2006gz. We estimate the ejected $^{56}$Ni mass of $1.2\pm 0.3$ $\Msun$ for no host extinction case (or 1.6$\pm$ 0.4 M$_{\odot}$ for the host extinction of $A_{V}=0.29$ mag). The C {\sc ii} $\lambda$6580 absorption line keeps visible until a week after maximum, which diminished in SN 2006gz before its maximum brightness. The line velocity of Si {\sc ii} $\lambda$6355 is about 8000 km s$^{-1}$ around the maximum, being considerably slower than that of SN 2006gz, while comparable to that of SN 2003fg. The velocity of the C {\sc ii} line is almost comparable to that of the Si {\sc ii}. The presence of the carbon line suggests that thick unburned C+O layers remain after the explosion. SN 2009dc is a plausible candidate of the super-Chandrasekhar mass SNe Ia.

Published
2009
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9. Site C0025

Author

Kimura, G., primary, Hirose, T., additional, Ikari, M., additional, Kanagawa, K., additional, Kinoshita, M., additional, Kitajima, H., additional, Saffer, D., additional, Tobin, H., additional, Yamaguchi, A., additional, Eguchi, N., additional, Maeda, L., additional, Toczko, S., additional, Bedford, J., additional, Chiyonobu, S., additional, Colson, T.A., additional, Conin, M., additional, Cornard, P.H., additional, Dielforder, A., additional, Doan, M.L., additional, Dutilleul, J., additional, Faulkner, D.R., additional, Fukuchi, R., additional, Guérin, G., additional, Hamada, Y., additional, Hamahashi, M., additional, Hong, W.L., additional, Ijiri, A., additional, Jaeger, D., additional, Jeppson, T., additional, Jin, Z., additional, John, B.E., additional, Kitamura, M., additional, Kopf, A., additional, Masuda, H., additional, Matsuoka, A., additional, Moore, G.F., additional, Otsubo, M., additional, Regalla, C., additional, Sakaguchi, A., additional, Sample, J., additional, Schleicher, A., additional, Sone, H., additional, Stanislowski, K., additional, Strasser, M., additional, Toki, T., additional, Tsuji, T., additional, Ujiie, K., additional, Underwood, M.B., additional, Yabe, S., additional, Yamamoto, Y., additional, Zhang, J., additional, Sanada, Y., additional, Kido, Y., additional, Le Ber, E., additional, and Saito, S., additional

Published
2020
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10. Site C0002

Author

Kitajima, H., primary, Hirose, T., additional, Ikari, M., additional, Kanagawa, K., additional, Kimura, G., additional, Kinoshita, M., additional, Saffer, D., additional, Tobin, H., additional, Yamaguchi, A., additional, Eguchi, N., additional, Maeda, L., additional, Toczko, S., additional, Bedford, J., additional, Chiyonobu, S., additional, Colson, T.A., additional, Conin, M., additional, Cornard, P.H., additional, Dielforder, A., additional, Doan, M.L., additional, Dutilleul, J., additional, Faulkner, D.R., additional, Fukuchi, R., additional, Guérin, G., additional, Hamada, Y., additional, Hamahashi, M., additional, Hong, W.L., additional, Ijiri, A., additional, Jaeger, D., additional, Jeppson, T., additional, Jin, Z., additional, John, B.E., additional, Kitamura, M., additional, Kopf, A., additional, Masuda, H., additional, Matsuoka, A., additional, Moore, G.F., additional, Otsubo, M., additional, Regalla, C., additional, Sakaguchi, A., additional, Sample, J., additional, Schleicher, A., additional, Sone, H., additional, Stanislowski, K., additional, Strasser, M., additional, Toki, T., additional, Tsuji, T., additional, Ujiie, K., additional, Underwood, M.B., additional, Yabe, S., additional, Yamamoto, Y., additional, Zhang, J., additional, Sanada, Y., additional, Kido, Y., additional, Le Ber, E., additional, and Saito, S., additional

Published
2020
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11. Expedition 358 summary

Author

Tobin, H., primary, Hirose, T., additional, Ikari, M., additional, Kanagawa, K., additional, Kimura, G., additional, Kinoshita, M., additional, Kitajima, H., additional, Saffer, D., additional, Yamaguchi, A., additional, Eguchi, N., additional, Maeda, L., additional, Toczko, S., additional, Bedford, J., additional, Chiyonobu, S., additional, Colson, T.A., additional, Conin, M., additional, Cornard, P.H., additional, Dielforder, A., additional, Doan, M.L., additional, Dutilleul, J., additional, Faulkner, D.R., additional, Fukuchi, R., additional, Guérin, G., additional, Hamada, Y., additional, Hamahashi, M., additional, Hong, W.L., additional, Ijiri, A., additional, Jaeger, D., additional, Jeppson, T., additional, Jin, Z., additional, John, B.E., additional, Kitamura, M., additional, Kopf, A., additional, Masuda, H., additional, Matsuoka, A., additional, Moore, G.F., additional, Otsubo, M., additional, Regalla, C., additional, Sakaguchi, A., additional, Sample, J., additional, Schleicher, A., additional, Sone, H., additional, Stanislowski, K., additional, Strasser, M., additional, Toki, T., additional, Tsuji, T., additional, Ujiie, K., additional, Underwood, M.B., additional, Yabe, S., additional, Yamamoto, Y., additional, Zhang, J., additional, Sanada, Y., additional, Kido, Y., additional, Le Ber, E., additional, and Saito, S., additional

Published
2020
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12. Expedition 358 methods

Author

Hirose, T., primary, Ikari, M., additional, Kanagawa, K., additional, Kimura, G., additional, Kinoshita, M., additional, Kitajima, H., additional, Saffer, D., additional, Tobin, H., additional, Yamaguchi, A., additional, Eguchi, N., additional, Maeda, L., additional, Toczko, S., additional, Bedford, J., additional, Chiyonobu, S., additional, Colson, T.A., additional, Conin, M., additional, Cornard, P.H., additional, Dielforder, A., additional, Doan, M.L., additional, Dutilleul, J., additional, Faulkner, D.R., additional, Fukuchi, R., additional, Guérin, G., additional, Hamada, Y., additional, Hamahashi, M., additional, Hong, W.L., additional, Ijiri, A., additional, Jaeger, D., additional, Jeppson, T., additional, Jin, Z., additional, John, B.E., additional, Kitamura, M., additional, Kopf, A., additional, Masuda, H., additional, Matsuoka, A., additional, Moore, G.F., additional, Otsubo, M., additional, Regalla, C., additional, Sakaguchi, A., additional, Sample, J., additional, Schleicher, A., additional, Sone, H., additional, Stanislowski, K., additional, Strasser, M., additional, Toki, T., additional, Tsuji, T., additional, Ujiie, K., additional, Underwood, M.B., additional, Yabe, S., additional, Yamamoto, Y., additional, Zhang, J., additional, Sanada, Y., additional, Kido, Y., additional, Le Ber, E., additional, and Saito, S., additional

Published
2020
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13. Site C0024

Author

Yamaguchi, A., primary, Hirose, T., additional, Ikari, M., additional, Kanagawa, K., additional, Kimura, G., additional, Kinoshita, M., additional, Kitajima, H., additional, Saffer, D., additional, Tobin, H., additional, Eguchi, N., additional, Maeda, L., additional, Toczko, S., additional, Bedford, J., additional, Chiyonobu, S., additional, Colson, T.A., additional, Conin, M., additional, Cornard, P.H., additional, Dielforder, A., additional, Doan, M.L., additional, Dutilleul, J., additional, Faulkner, D.R., additional, Fukuchi, R., additional, Guérin, G., additional, Hamada, Y., additional, Hamahashi, M., additional, Hong, W.L., additional, Ijiri, A., additional, Jaeger, D., additional, Jeppson, T., additional, Jin, Z., additional, John, B.E., additional, Kitamura, M., additional, Kopf, A., additional, Masuda, H., additional, Matsuoka, A., additional, Moore, G.F., additional, Otsubo, M., additional, Regalla, C., additional, Sakaguchi, A., additional, Sample, J., additional, Schleicher, A., additional, Sone, H., additional, Stanislowski, K., additional, Strasser, M., additional, Toki, T., additional, Tsuji, T., additional, Ujiie, K., additional, Underwood, M.B., additional, Yabe, S., additional, Yamamoto, Y., additional, Zhang, J., additional, Sanada, Y., additional, Kido, Y., additional, Le Ber, E., additional, and Saito, S., additional

Published
2020
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14. Discovery of a WZ Sge-Type Dwarf Nova, SDSS J102146.44+234926.3: Unprecedented Infrared Activity during a Rebrightening Phase

Author

Uemura, M., Arai, A., Krajci, T., Pavlenko, E., Shugarov, S. Yu., Katysheva, N. A., Goranskij, V. P., Maehara, H., Imada, A., Kato, T., Nogami, D., Nakajima, K., Ohsugi, T., Yamashita, T., Kawabata, K. S., Nagae, O., Chiyonobu, S., Fukazawa, Y., Mizuno, T., Katagiri, H., Takahashi, H., Ueda, A., Hayashi, T., Okita, K., Yoshida, M., Yanagisawa, K., Sato, S., Kino, M., and Sadakane, K.

Subjects
Astrophysics
Abstract

Several SU UMa-type dwarf novae, in particular, WZ Sge-type stars tend to exhibit rebrightenings after superoutbursts. The rebrightening phenomenon is problematic for the disk instability theory of dwarf novae since it requires a large amount of remnant matter in the disk even after superoutbursts. Here, we report our optical and infrared observations during the first-ever outburst of a new dwarf nova, SDSS J102146.44+234926.3. During the outburst, we detected superhumps with a period of 0.056281 +/- 0.000015 d, which is typical for superhump periods in WZ Sge stars. In conjunction with the appearance of a long-lived rebrightening, we conclude that the object is a new member of WZ Sge stars. Our observations, furthermore, revealed infrared behaviors for the first time in the rebrightening phase of WZ Sge stars. We discovered prominent infrared superhumps. We calculate the color temperature of the infrared superhump source to be 4600-6400 K. These temperatures are too low to be explained with a fully-ionized disk appearing during dwarf nova outbursts. We also found a Ks-band excess over the hot disk component. These unprecedented infrared activities provide evidence for the presence of mass reservoir at the outermost part of the accretion disk. We propose that a moderately high mass-accretion rate at this infrared active region leads to the long-lived rebrightening observed in SDSS J102146.44+234926.3., Comment: 11 pages, 10 figures. Accepted for publication in PASJ

Published
2007
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15. Site C0010

Author

Saffer, D., primary, Kopf, A., additional, Toczko, S., additional, Araki, E., additional, Carr, S., additional, Kimura, T., additional, Kinoshita, C., additional, Kobayashi, R., additional, Machida, Y., additional, Rösner, A., additional, Wallace, L.M., additional, Chiyonobu, S., additional, Kanagawa, K., additional, Kanamatsu, T., additional, Kimura, G., additional, and Underwood, M.B., additional

Published
2017
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16. Expedition 365 summary

Author

Kopf, A., primary, Saffer, D., additional, Toczko, S., additional, Araki, E., additional, Carr, S., additional, Kimura, T., additional, Kinoshita, C., additional, Kobayashi, R., additional, Machida, Y., additional, Rösner, A., additional, Wallace, L.M., additional, Chiyonobu, S., additional, Kanagawa, K., additional, Kanamatsu, T., additional, Kimura, G., additional, and Underwood, M.B., additional

Published
2017
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17. Expedition 365 methods

Author

Saffer, D., primary, Kopf, A., additional, Toczko, S., additional, Araki, E., additional, Carr, S., additional, Kimura, T., additional, Kinoshita, C., additional, Kobayashi, R., additional, Machida, Y., additional, Rösner, A., additional, Wallace, L.M., additional, Chiyonobu, S., additional, Kanagawa, K., additional, Kanamatsu, T., additional, Kimura, G., additional, and Underwood, M.B., additional

Published
2017
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25. OPTICAL AND NEAR-INFRARED POLARIMETRY OF HIGHLY REDDENED Type Ia SUPERNOVA 2014J: PECULIAR PROPERTIES OF DUST IN M82

Author

Kawabata, K. S., primary, Akitaya, H., additional, Yamanaka, M., additional, Itoh, R., additional, Maeda, K., additional, Moritani, Y., additional, Ui, T., additional, Kawabata, M., additional, Mori, K., additional, Nogami, D., additional, Nomoto, K., additional, Suzuki, N., additional, Takaki, K., additional, Tanaka, M., additional, Ueno, I., additional, Chiyonobu, S., additional, Harao, T., additional, Matsui, R., additional, Miyamoto, H., additional, Nagae, O., additional, Nakashima, A., additional, Nakaya, H., additional, Ohashi, Y., additional, Ohsugi, T., additional, Komatsu, T., additional, Sakimoto, K., additional, Sasada, M., additional, Sato, H., additional, Tanaka, H., additional, Urano, T., additional, Yamashita, T., additional, Yoshida, M., additional, Arai, A., additional, Ebisuda, N., additional, Fukazawa, Y., additional, Fukui, A., additional, Hashimoto, O., additional, Honda, S., additional, Izumiura, H., additional, Kanda, Y., additional, Kawaguchi, K., additional, Kawai, N., additional, Kuroda, D., additional, Masumoto, K., additional, Matsumoto, K., additional, Nakaoka, T., additional, Takata, K., additional, Uemura, M., additional, and Yanagisawa, K., additional

Published
2014
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26. GRB 091208B: FIRST DETECTION OF THE OPTICAL POLARIZATION IN EARLY FORWARD SHOCK EMISSION OF A GAMMA-RAY BURST AFTERGLOW

Author

Uehara, T., primary, Toma, K., additional, Kawabata, K. S., additional, Chiyonobu, S., additional, Fukazawa, Y., additional, Ikejiri, Y., additional, Inoue, T., additional, Itoh, R., additional, Komatsu, T., additional, Miyamoto, H., additional, Mizuno, T., additional, Nagae, O., additional, Nakaya, H., additional, Ohsugi, T., additional, Sakimoto, K., additional, Sasada, M., additional, Tanaka, H., additional, Uemura, M., additional, Yamanaka, M., additional, Yamashita, T., additional, Yamazaki, R., additional, and Yoshida, M., additional

Published
2012
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27. Rapidly-Responding Optical Polarimetry of GRB afterglows with Hiroshima 1.5-m Telescope and One-shot Wide-field Polarimeter

Author

Kawabata, K. S., primary, Uehara, T., additional, Yamanaka, M., additional, Sasada, M., additional, Ikejiri, Y., additional, Itoh, R., additional, Komatsu, T., additional, Uemura, M., additional, Nagae, O., additional, Chiyonobu, S., additional, Tanaka, H., additional, Ohsugi, T., additional, Fukazawa, Y., additional, Mizuno, T., additional, Katagiri, H., additional, Takahashi, H., additional, Miyamoto, H., additional, Sakimoto, K., additional, Hiragi, K., additional, Yoshida, M., additional, Yamazaki, R., additional, Toma, K., additional, Arai, A., additional, Isogai, M., additional, Nakaya, H., additional, Kamata, Y., additional, Miyazaki, S., additional, Yamashita, T., additional, Suzuki, M., additional, Sato, S., additional, Kawai, Nobuyuki, additional, and Nagataki, Shigehiro, additional

Published
2010
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28. EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

Author

Yamanaka, M., primary, Kawabata, K. S., additional, Kinugasa, K., additional, Tanaka, M., additional, Imada, A., additional, Maeda, K., additional, Nomoto, K., additional, Arai, A., additional, Chiyonobu, S., additional, Fukazawa, Y., additional, Hashimoto, O., additional, Honda, S., additional, Ikejiri, Y., additional, Itoh, R., additional, Kamata, Y., additional, Kawai, N., additional, Komatsu, T., additional, Konishi, K., additional, Kuroda, D., additional, Miyamoto, H., additional, Miyazaki, S., additional, Nagae, O., additional, Nakaya, H., additional, Ohsugi, T., additional, Omodaka, T., additional, Sakai, N., additional, Sasada, M., additional, Suzuki, M., additional, Taguchi, H., additional, Takahashi, H., additional, Tanaka, H., additional, Uemura, M., additional, Yamashita, T., additional, Yanagisawa, K., additional, and Yoshida, M., additional

Published
2009
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30. Three Advantages of the KANATA 1.5-m Telescope as a Powerful Partner for GLAST

Author

Uemura, M., primary, Ohsugi, T., additional, Yamashita, T., additional, Kawabata, K., additional, Arai, A., additional, Nagae, O., additional, Chiyonobu, S., additional, Ueda, A., additional, Fukazawa, Y., additional, Mizuno, T., additional, Katagiri, H., additional, Takahashi, H., additional, Hayashi, T., additional, Okita, K., additional, Yoshida, M., additional, Yanagisawa, K., additional, Sato, S., additional, Kino, M., additional, Kitagawa, M., additional, and Sadakane, K., additional

Published
2007
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32. OutcropHyBNet: Hybrid Backbone Networks with Data Augmentation for Accurate Stratum Semantic Segmentation of Monocular Outcrop Images in Carbon Capture and Storage Applications.

Author

Madokoro H, Sato K, Nix S, Chiyonobu S, Nagayoshi T, and Sato K

Abstract

The rapid advancement of climate change and global warming have widespread impacts on society, including ecosystems, water security, food production, health, and infrastructure. To achieve significant global emission reductions, approximately 74% is expected to come from cutting carbon dioxide (CO2) emissions in energy supply and demand. Carbon Capture and Storage (CCS) has attained global recognition as a preeminent approach for the mitigation of atmospheric carbon dioxide levels, primarily by means of capturing and storing CO2 emissions originating from fossil fuel systems. Currently, geological models for storage location determination in CCS rely on limited sampling data from borehole surveys, which poses accuracy challenges. To tackle this challenge, our research project focuses on analyzing exposed rock formations, known as outcrops, with the goal of identifying the most effective backbone networks for classifying various strata types in outcrop images. We leverage deep learning-based outcrop semantic segmentation techniques using hybrid backbone networks, named OutcropHyBNet, to achieve accurate and efficient lithological classification, while considering texture features and without compromising computational efficiency. We conducted accuracy comparisons using publicly available benchmark datasets, as well as an original dataset expanded through random sampling of 13 outcrop images obtained using a stationary camera, installed on the ground. Additionally, we evaluated the efficacy of data augmentation through image synthesis using Only Adversarial Supervision for Semantic Image Synthesis (OASIS). Evaluation experiments on two public benchmark datasets revealed insights into the classification characteristics of different classes. The results demonstrate the superiority of Convolutional Neural Networks (CNNs), specifically DeepLabv3, and Vision Transformers (ViTs), particularly SegFormer, under specific conditions. These findings contribute to advancing accurate lithological classification in geological studies using deep learning methodologies. In the evaluation experiments conducted on ground-level images obtained using a stationary camera and aerial images captured using a drone, we successfully demonstrated the superior performance of SegFormer across all categories.

Published
2023
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33. Development of Drone-Mounted Multiple Sensing System with Advanced Mobility for In Situ Atmospheric Measurement: A Case Study Focusing on PM 2.5 Local Distribution.

Author

Madokoro H, Kiguchi O, Nagayoshi T, Chiba T, Inoue M, Chiyonobu S, Nix S, Woo H, and Sato K

Subjects
Environmental Monitoring, Particulate Matter analysis, Air Pollutants analysis, Air Pollution analysis
Abstract

This study was conducted using a drone with advanced mobility to develop a unified sensor and communication system as a new platform for in situ atmospheric measurements. As a major cause of air pollution, particulate matter (PM) has been attracting attention globally. We developed a small, lightweight, simple, and cost-effective multi-sensor system for multiple measurements of atmospheric phenomena and related environmental information. For in situ local area measurements, we used a long-range wireless communication module with real-time monitoring and visualizing software applications. Moreover, we developed four prototype brackets with optimal assignment of sensors, devices, and a camera for mounting on a drone as a unified system platform. Results of calibration experiments, when compared to data from two upper-grade PM2.5 sensors, demonstrated that our sensor system followed the overall tendencies and changes. We obtained original datasets after conducting flight measurement experiments at three sites with differing surrounding environments. The experimentally obtained prediction results matched regional PM2.5 trends obtained using long short-term memory (LSTM) networks trained using the respective datasets.

Published
2021
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