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1,968 results on '"Yanagisawa, K."'

1. Spark plasma sintering of hydrothermally derived ultrafine Ca doped lanthanum chromite powders

Author: Rendón-Angeles, J. C., Rivas-Vázquez, L. P., Pech-Canul, M. I., López-Cuevas, J., Díaz de la Torre, S., Pena, P., and Yanagisawa, K.
Subjects: Lanthanum Chromite, Sintering, Solid Solution, Hydrothermal Treatment, Interconnector, Perovskites, Cromita de Lantano, Sinterización, Solución Sólida, Síntesis Hidrotermal, Interconector, Perovskitas, Clay industries. Ceramics. Glass, TP785-869
Abstract: Lanthanum chromite nano-particles, with a composition of La0.9Ca0.1CrO3 and La0.8Ca0.2CrO3, were produced by 1 h of hydrothermal reaction at 400 and 425°C respectively. The sintering of the powders was conducted using a spark plasma apparatus over the temperature range 1300-1550ºC for 1 min with a constant loading pressure of 45 MPa. Additional sintering experiments using conventional firing were carried out for comparison. Fully densified (98 % r.d.) lanthanum chromite pellets with fine equiaxial grains 2.3 μm in size were obtained using the SPS (spark plasma sintering) method. In contrast, a maximum relative density of 97 % was produced using La0.8Ca0.2CrO3 sintered conventionally at 1400ºC for 300 min, and the average grain size of the resulting sintered sample was 6 μm.Partículas ultrafinas de cromita de lantano, con una composición de La0.9Ca0.1CrO3 y La0.8Ca0.2CrO3, se obtuvieron después de 1 hora de síntesis hidrotermal a las temperaturas de 400 y 425°C respectivamente. Los compuestos obtenidos, con un tamaño de partícula de ~ 200 nm, se caracterizaron utilizando las técnicas de DRX, MEB y MET. La sinterización de estos polvos se efectuó en un equipo de chispa de plasma en el rango de temperatura de 1300-1500°C durante 1 min, y a una presión de compactación de 45 MPa. Ambos polvos también se sinterizaron siguiendo un tratamiento térmico convencional, en aire, con el propósito de comparar ambos métodos de sinterización. Las muestras de cromita de lantano sinterizadas por plasma presentaban una densidad relativa del 98 % (/t); y una microestructura monofásica con granos equaxiales con un tamaño medio de grano menor de 2.3 μm. En contraste, la composición La0.8Ca0.2CrO3, sinterizada a 1400°C/300 min, por métodos convencionales alcanzó una densidad relativa máxima del 97 % y su microestructura estaba formada por una sola fase con un tamaño medio de grano de 6 μm.
Published: 2006

2. Kojima-1Lb Is a Mildly Cold Neptune around the Brightest Microlensing Host Star

Author: Fukui, A., Suzuki, D., Koshimoto, N., Bachelet, E., Vanmunster, T., Storey, D., Maehara, H., Yanagisawa, K., Yamada, T., Yonehara, A., Hirano, T., Bennett, D. P., Bozza, V., Mawet, D., Penny, M. T., Awiphan, S., Oksanen, A., Heintz, T. M., Oberst, T. E., Bejar, V. J. S., Casasayas-Barris, N., Chen, G., Crouzet, N., Hidalgo, D., Klagyivik, P., Murgas, F., Narita, N., Palle, E., Parviainen, H., Watanabe, N., Kusakabe, N., Mori, M., Terada, Y., de Leon, J. P., Hernandez, A., Luque, R., Monelli, M., Montanes-Rodriguez, P., Prieto-Arranz, J., Murata, K. L., Shugarov, S., Kubota, Y., Otsuki, C., Shionoya, A., Nishiumi, T., Nishide, A., Fukagawa, M., Onodera, K., Villanueva Jr., S., Street, R. A., Tsapras, Y., Hundertmark, M., Kuzuhara, M., Fujita, M., Beichman, C., Beaulieu, J. -P., Alonso, R., Kawai, D. E. Reichart N., and Tamura, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report the analysis of additional multiband photometry and spectroscopy and new adaptive optics (AO) imaging of the nearby planetary microlensing event TCP J05074264+2447555 (Kojima-1), which was discovered toward the Galactic anticenter in 2017 (Nucita et al.). We confirm the planetary nature of the light-curve anomaly around the peak while finding no additional planetary feature in this event. We also confirm the presence of apparent blending flux and the absence of significant parallax signal reported in the literature. The AO image reveals no contaminating sources, making it most likely that the blending flux comes from the lens star. The measured multiband lens flux, combined with a constraint from the microlensing model, allows us to narrow down the previously unresolved mass and distance of the lens system. We find that the primary lens is a dwarf on the K/M boundary (0.581 \pm 0.033 M_sun) located at 505 \pm 47 pc and the companion (Kojima-1Lb) is a Neptune-mass planet (20.0 \pm 2.0 M_earth) with a semi-major axis of 1.08 ^{+0.62}_{-0.18} au. This orbit is a few times smaller than those of typical microlensing planets and is comparable to the snow-line location at young ages. We calculate that the a priori detection probability of Kojima-1Lb is only \sim 35%, which may imply that Neptunes are common around the snow line, as recently suggested by the transit and radial velocity techniques. The host star is the brightest among the microlensing planetary systems (Ks = 13.7), offering a great opportunity to spectroscopically characterize this system, even with current facilities., Comment: 27 pages, 12 figures, published in Astronomical Journal
Published: 2019
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3. Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - X. Three high-contrast systems with secondaries detected with IR spectroscopy

Author: Hełminiak, K. G., Tokovinin, A., Niemczura, E., Pawłaszek, R., Yanagisawa, K., Brahm, R., Espinoza, N., Ukita, N., Ratajczak, E. Kambe. M., Hempel, M., Jordán, A., Konacki, M., Sybilski, P., Kozłowski, S. K., Litwickim, M., and Tamura, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present results of the combined photometric and spectroscopic analysis of three detached eclipsing binaries, which secondary components are not visible or very hard to identify in the optical spectra - ASAS J052743-0359.7, ASAS J065134-2211.5, and ASAS J073507-0905.7. The first one is a known visual binary ADS 4022, and we found that it is a quadruple system, composed of two spectroscopic binaries, one of which shows eclipses. None of the systems was previously recognized as a spectroscopic binary. We collected a number of high-resolution optical and IR spectra to calculate the radial velocities (RVs) and later combined them with MITSuME and ASAS photometry. The IR spectra were crucial for secure identification of the cooler components' lines. RV measurements were done with the TODCOR technique, and RV curves modelled with our own procedure V2FIT. Light curve modelling was performed with JKTEBOP and PHOEBE codes. Temperatures and metallicities of two systems were estimated from spectra. For the ADS 4022 system we also used the archival WDS data and new SOAR observations in order to derive the orbit of the visual pair for the first time. Ages were estimated by comparing our results with PARSEC isochrones. The eclipsing pair A052743 A ($P=5.27$ d) is composed of a 1.03(6) M$_\odot$, 1.03(2) R$_\odot$ primary and a 0.60(2) M$_\odot$, 0.59(2) R$_\odot$ secondary. The components of the $P=21.57$ d non-eclipsing pair B likely have masses in between the two eclipsing components, and both pairs are on a $\sim$188 yr orbit around their common centre of mass. The system A065134 ($P=8.22$ d) consists of a 0.956(12) M$_\odot$, 0.997(4) R$_\odot$ primary and a 0.674(5) M$_\odot$, 0.690(7) R$_\odot$ secondary. Finally, A073507 ($P=1.45$ d), which consists of a 1.452(34) M$_\odot$, 1.635(12) R$_\odot$ primary and a 0.808(13) M$_\odot$, 0.819(11) R$_\odot$ secondary, is likely a PMS system., Comment: 22 pages, 13 figures, 8 tables, accepted for publication in A&A, abstract modified for arXiv
Published: 2018
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4. Optical and Near-Infrared Polarimetry of Non-Periodic Comet C/2013 US10 (Catalina)

Author: Kwon, Y. G., Ishiguro, M., Kuroda, D., Hanayama, H., Kawabata, K. S., Akitaya, H., Nakaoka, T., Itoh, R., Toda, H., Yanagisawa, K., Lee, M. -G., Ohta, K., Yoshida, M., Kawai, N., and Watanabe, J. -I.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present an optical and near-infrared (hereafter NIR) polarimetric study of a comet C/2013 US10 (Catalina) observed on UT 2015 December 17-18 at phase angles of $\alpha$=52.1 deg - 53.1 deg. Additionally, we obtained an optical spectrum and multi-band images to examine the influence of gas emission. We find that the observed optical signals are significantly influenced by gas emission, that is, the gas-to-total intensity ratio varies from 5 to 30 % in the $R_{\rm C}$ and 3 to 18 % in the $I_{\rm C}$ bands, depending on the position in the coma. We derive the `gas-free dust polarization degrees' of 13.8$\pm$1.0 % in the $R_{\rm C}$ and 12.5$\pm$1.1 % in the $I_{\rm C}$ bands and a gray polarimetric color, i.e., -8.7$\pm$9.9 % $\mu \mathrm{m}$$^{-1}$ in optical and 1.6$\pm$0.9 % $\mu \mathrm{m}$$^{-1}$ in NIR. The increments of polarization obtained from the gas correction show that the polarimetric properties of the dust in this low-polarization comet are not different from those in high-polarization comets. In this process, the cometocentric distance dependence of polarization has disappeared. We also find that the $R_{\rm C}$-band polarization degree of the southeast dust tail, which consists of large dust particles (100 $\mu \mathrm{m}$ - 1 mm), is similar to that in the outer coma where small and large ones are mixed. Our study confirms that the dichotomy of cometary polarization does not result from the difference of dust properties, but from depolarizing gas contamination. This conclusion can provide a strong support for similarity in origin of comets., Comment: 19 pages, 9 figures, Astronomical Journal (accepted on 2017 August 30)
Published: 2017
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5. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., De Rosa, R., DeSalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., MacDonald, T., Machenschalk, B., MacInnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McCormick, S., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McWilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal-Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492
Published: 2016
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6. Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864
Published: 2016
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7. Rapid one-pot hydrothermal reaction for preparing BaCu2Si2O7 fine particles with controlled blue colour tonality

Author: Rendón-Angeles, J.C., Quiñones-Gurrola, J.R., López-Cuevas, J., Gonzalez, L.A., Matamoros-Veloza, Z., Perez-Ramos, E., Yanagisawa, K., Tamayo, A., and Alonso, J.R.
Published: 2021
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8. Weight and cost reduction potentials with high performance polymers for gears

Author: Yanagisawa, K., primary and Weinmann, A., additional
Published: 2022
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9. 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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10. The detection of C60 in the well-characterized planetary nebula M1-11

Author: Otsuka, Masaaki, Kemper, F., Hyung, S., Sargent, B. A., Meixner, M., Tajitsu, A., and Yanagisawa, K.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We performed multiwavelength observations of the young planetary nebula (PN) M1-11 and obtained its elemental abundances, dust mass, and the evolutionary status of the central star. The AKARI/IRC, VLT/VISIR, and Spitzer/IRS spectra show features due to carbon-rich dust, such as the 3.3, 8.6, and 11.3 um features due to polycyclic aromatic hydrocarbons (PAHs), a smooth continuum attributable to amorphous carbon, and the broad 11.5 and 30 um features often ascribed to SiC and MgS, respectively. We also report the presence of an unidentified broad feature at 16-22 um, similar to the feature found in Magellanic Cloud PNe with either C-rich or O-rich gas-phase compositions. We identify for the first time in M1-11 spectral lines at 8.5 (blended with PAH), 17.3, and 18.9 um that we attribute to the C60 fullerene. This identification is strengthened by the fact that other Galactic PNe in which fullerenes are detected, have similar central stars, similar gas-phase abundances, and a similar dust composition to M1-11. The weak radiation field due to the relatively cool central stars in these PNe may provide favorable conditions for fullerenes to survive in the circumstellar medium. Using the photo-ionization code CLOUDY, combined with a modified blackbody, we have fitted the ~0.1-90 um spectral energy distribution and determined the dust mass in the nebula to be ~3.5x10^{-4} Msun$. Our chemical abundance analysis and SED model suggest that M1-11 is perhaps a C-rich PN with C/O ratio in the gas-phase of +0.19 dex, and that it evolved from a 1-1.5 Msun star., Comment: Accepted for publication by the Astrophysical Journal
Published: 2013
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11. The influence of initial gold nanoparticles layer on migration of silver nanoparticles in silver/glass matrix

Author: Kyaw, H.H., Myint, M.T.Z., Al-Harthi, S.H., Maekawa, T., Yanagisawa, K., Sellai, A., and Dutta, J.
Published: 2019
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12. Controllable synthesis of BaCuSi2O6 fine particles via a one-pot hydrothermal reaction with enhanced violet colour hue

Author: Corona-Martínez, D.A., Rendón-Angeles, J.C., Gonzalez, L.A., Matamoros-Veloza, Z., Yanagisawa, K., Tamayo, A., and Alonso, J.R.
Published: 2019
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13. The GRB 071112C: A Case Study of Different Mechanisms in X-ray and Optical Temporal Evolution

Author: Huang, K. Y., Urata, Y., Tung, Y. H., Lin, H. M., Xin, L. P., Yoshida, M., Zheng, W., Akerlof, C., Wang, S. Y., Ip, W. H., Lehner, M. J., Bianco, F. B., Kawai, N., Kuroda, D., Marshall, S. L., Schwamb, M. E., Qiu, Y., Wang, J. H., Wen, C. Y., Wei, J., Yanagisawa, K., and Zhang, Z. W.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the study on GRB 071112C X-ray and optical light curves. In these two wavelength ranges, we have found different temporal properties. The R-band light curve showed an initial rise followed by a single power-law decay, while the X-ray light curve was described by a single power-law decay plus a flare-like feature. Our analysis shows that the observed temporal evolution cannot be described by the external shock model in which the X-ray and optical emission are produced by the same emission mechanism. No significant color changes in multi-band light curves and a reasonable value of the initial Lorentz factor ({\Gamma}0 = 275 \pm 20) in a uniform ISM support the afterglow onset scenario as the correct interpretation for the early R-band rise. The result suggests the optical flux is dominated by afterglow. Our further investigations show that the X-ray flux could be created by an additional feature related to energy injection and X-ray afterglow. Different theoretical interpretations indicate the additional feature in X-ray can be explained by either late internal dissipation or local inverse-Compton scattering in the external shock., Comment: 20 pages, 3 figures, accepted for publication in ApJ
Published: 2012
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14. OAO/ISLE Near-IR Spectroscopy of IRAS Galaxies

Author: Matsuoka, Y., Yuan, F. -T., Takeuchi, Y., and Yanagisawa, K.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the results of the near-infrared (IR) spectroscopy of nine IRAS galaxies (NGC 1266, NGC 1320, NGC 2633, NGC 2903, NGC 3034, Mrk 33, NGC 7331, NGC 7625, NGC 7714) with the ISLE imager and spectrograph mounted on the Okayama Astrophysical Observatory 1.88 m telescope. [Fe II] 1.257 um and Pa beta emission lines were observed for the whole sample while H2 2.121 um and Br gamma lines were additionally obtained for two sources, whose flux ratios are used as a diagnostic tool of dominant energy sources of the galaxies. We find that the nucleus of NGC 1266 is most likely a low ionization nuclear emission-line region (LINER), while NGC 2633 and NGC 2903 possibly harbor active galactic nuclei (AGNs). No AGN or LINER signal is found for other objects. In addition, we find the spectral features which is indicative of some unusual phenomena occurring in the galaxies, such as the large [Fe II] line widths compared to the local escape velocity in NGC 1266. The present work shows the potential ability of the ISLE to shed new light on the nature of infrared galaxies, either through a statistical survey of galaxies or an exploration of spectral features found in individual objects., Comment: Accepted for publication in PASJ
Published: 2011
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15. Thermo-physical properties of 162173 (1999 JU3), a potential flyby and rendezvous target for interplanetary missions

Author: Mueller, T. G., Durech, J., Hasegawa, S., Abe, M., Kawakami, K., Kasuga, T., Kinoshita, D., Kuroda, D., Urakawa, S., Okumura, S., Sarugaku, Y., Miyasaka, S., Takagi, Y., Weissman, P. R., Choi, Y. -J., Larson, S., Yanagisawa, K., and Nagayama, S.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Near-Earth asteroid 162173 (1999 JU3) is a potential flyby and rendezvous target for interplanetary missions because of its easy to reach orbit. The physical and thermal properties of the asteroid are relevant for establishing the scientific mission goals and also important in the context of near-Earth object studies in general. Our goal was to derive key physical parameters such as shape, spin-vector, size, geometric albedo, and surface properties of 162173 (1999 JU3). With three sets of published thermal observations (ground-based N-band, Akari IRC, Spitzer IRS), we applied a thermophysical model to derive the radiometric properties of the asteroid. The calculations were performed for the full range of possible shape and spin-vector solutions derived from the available sample of visual lightcurve observations. The near-Earth asteroid 162173 (1999 JU3) has an effective diameter of 0.87 +/- 0.03 km and a geometric albedo of 0.070 +/- 0.006. The chi2-test reveals a strong preference for a retrograde sense of rotation with a spin-axis orientation of lambda_ecl = 73 deg, beta_ecl = -62 deg and P_sid = 7.63 +/- 0.01 h. The most likely thermal inertia ranges between 200 and 600 Jm-2s-0.5K-1, about a factor of 2 lower than the value for 25143 Itokawa. This indicates that the surface lies somewhere between a thick-dust regolith and a rock/boulder/cm-sized, gravel-dominated surface like that of 25143 Itokawa. Our analysis represents the first time that shape and spin-vector information has been derived from a combined data set of visual lightcurves (reflected light) and mid-infrared photometry and spectroscopy (thermal emission)., Comment: 6 pages, 5 figures, 2 tables, accepted for publication in A&A (date of acceptance 05/Nov/2010)
Published: 2010
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16. Optical and Near-Infrared Photometric Observation during the Superoutburst of the WZ Sge-Type Dwarf Nova, V455 Andromedae

Author: Matsui, R., Uemura, M., Arai, A., Sasada, M., Ohsugi, T., Yamashita, T., Kawabata, K. S., Fukazawa, Y., Mizuno, T., Katagiri, H., Takahashi, H., Sato, S., Kino, M., Yoshida, M., Shimizu, Y., Nagayama, S., Yanagisawa, K., Toda, H., Okita, K., and Kawai, N.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We report on optical and infrared photometric observations of a WZ Sge-type dwarf nova, V455 And during a superoutburst in 2007. These observations were performed with the KANATA (V, J, and K_s bands) and MITSuME (g', Rc, and Ic bands) telescopes. Our 6-band simultaneous observations allowed us to investigate the temporal variation of the temperature and the size of the emitting region associated with the superoutburst and short-term modulations, such as early and ordinary superhumps. A hot (>11000 K) accretion disk suddenly disappeared when the superoutburst finished, while blackbody emission, probably from the disk, still remained dominant in the optical region with a moderately high temperature (~8000 K). This indicates that a substantial amount of gas was stored in the disk even after the outburst. This remnant matter may be a sign of an expected mass-reservoir which can trigger echo outbursts observed in several WZ Sge stars. The color variation associated with superhumps indicates that viscous heating in a superhump source stopped on the way to the superhump maximum, and a subsequent expansion of a low-temperature region made the maximum. The color variation of early superhumps was totally different from that of superhumps: the object was bluest at the early superhump minimum. The temperature of the early superhump light source was lower than that of an underlying component, indicating that the early superhump light source was a vertically expanded low-temperature region at the outermost part of the disk., Comment: 14 pages, 12 figures, PASJ accepted
Published: 2009
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17. 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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18. Simultaneous MITSuME gRI monitoring of S5 0716+714

Author: Stalin, C. S., Kawabata, K. S., Uemura, M., Yoshida, M., Kawai, N., Yanagisawa, K., Shimizu, Y., Kuroda, D., Nagayama, S., and Toda, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present results of our intra-night optical flux monitoring observations of S5 0716+714 done simultaneously in gRI filters. The observations were done using Multicolor Imaging Telescopes for Survey and Monstrous Explosions (MITSuME) instrument on the 50 cm telescope at the Okayama Astrophysical Observatory over 30 nights between 11 March 2008 and 8 May 2008. Of these 30 nights, 22 nights have continuous (without any break) observations with duration ranging from 1 to 6 hours and hence were considered for intra-night optical variability (INOV). In total we have 4888 datapoints which were simultaneous in gR and I filters. Of the 22 nights considered for INOV, the object showed flux variability on 19 nights with the amplitude of variability in the I-band ranging from ~4% to ~55%. The duty cycle for INOV was thus found to be 83%. No time lag between different bands was noticed on most of the nights, except for 3 nights where the variation in g was found to lead that of the I band by 0.3 to 1.5 hrs. On inter-night timescales, no lag was found between g and I bands. On inter-night timescales as well as intra-night timescales on most of the nights, the amplitude of variability was found to increase toward shorter wavelengths. The flux variations in the different bands were not achromatic, with the blazar tending to become bluer when brighter both on inter-night and intra-night timescales; and this might be attributed to the larger amplitude variation at shorter wavelengths. A clear periodic variation of 3.3 hrs was found on 1 April 2008 and a hint for another possible periodic variability of 4 hrs was found on 31 March 2008. During our 30 days of observations over a 2 month period the source has varied with an amplitude of variability as large as ~80%., Comment: 11 pages, 8 figures and 5 tables, Accepted in MNRAS
Published: 2009
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19. Laparoscopic liver resection for liver metastsis of colorectal cancer

Author: Muneta, M., primary, Ohmura, Y., additional, Takeda, Y., additional, Shinke, G., additional, Kinoshita, M., additional, Katsura, Y., additional, Yanagisawa, K., additional, Katsuyama, S., additional, Ikeshima, R., additional, Hiraki, M., additional, Sugimura, K., additional, Masuzawa, T., additional, Hata, T., additional, and Murata, K., additional
Published: 2024
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20. 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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21. MITSuME--Multicolor Imaging Telescopes for Survey and Monstrous Explosions

Author: Kotani, T., Kawai, N., Yanagisawa, K., Watanabe, J., Arimoto, M., Fukushima, H., Hattori, T., Inata, M., Izumiura, H., Kataoka, J., Koyano, H., Kubota, K., Kuroda, D., Mori, M., Nagayama, S., Ohta, K., Okada, T., Okita, K., Sato, R., Serino, Y., Shimizu, Y., Shimokawabe, T., Suzuki, M., Toda, H., Ushiyama, T., Yatsu, Y., Yoshida, A., and Yoshida, M.
Subjects: Astrophysics
Abstract: Development of MITSuME is reported. Two 50-cm optical telescopes have been built at Akeno in Yamanashi prefecture and at Okayama Astrophysical Observatory (OAO) in Okayama prefecture. Three CCD cameras for simultaneous g'RcIc photometry are to be mounted on each focal plane, covering a wide FOV of about 30" x 30". The limiting magnitude at V is fainter than 18. In addition to these two optical telescopes, a 91-cm IR telescope with a 1 deg x 1 deg field of view is being built at OAO, which performs photometry in YJHK bands. These robotic telescopes can start the observation of counterparts of a GRB within a minute from an alert. We aim to obtain photometric redshifts exceeding 10 with these telescopes. The performance and the current construction status of the telescopes are presented., Comment: 4 pages, 3 figures, 4th Workshop on Gamma-Ray Burst in the Afterglow Era, Roma, October 18-22, 2004
Published: 2007
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22. Observation Campaign of SS 433 in April 2006

Author: Kotani, T., Kubota, K., Namiki, M., Kawai, N., Ueda, Y., Trushkin, S., Fabrika, S., Afanasiev, V., Abolmasov, P., Kinugasa, K., Nagata, T., Irsmambetova, T., Tsukagoshi, T., Nakanishi, K., Tsuboi, M., Ozaki, S., Yanagisawa, K., Nishiyama, S., Shimokawabe, T., Yatsu, Y., Ishimura, T., and Fujisawa, K.
Subjects: Astrophysics
Abstract: A radio-IR-optical-X-ray observation campaign of SS 433 has been performed in April 2006, when the jet axis is almost perpendicular to the line of sight. Five flares have been detected during the campaign by radio monitoring observation with RATAN-600. The X-ray astronomical satellite Suzaku observed the source in and out of eclipse. In the X-ray data out of eclipse, the flux shows a significant variation with a time scale of hours. The source seems to be in the active state during the campaign. The observation logs and preliminary results are presented., Comment: 9 pages, 9 figures, to appear in proceedings of ``VI Microquasar Workshop: Microquasars and Beyond''
Published: 2006

23. Time–frequency-based non-harmonic analysis to reduce line-noise impact for LIGO observation system

Author: Jia, D., Yanagisawa, K., Hasegawa, M., Hirobayashi, S., Tagoshi, H., Narikawa, T., Uchikata, N., and Takahashi, H.
Published: 2018
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24. Earliest detection of the optical afterglow of GRB 030329 and its variability

Author: Sato, R., Kawai, N., Suzuki, M., Yatsu, Y., Kataoka, J., Takagi, R., Yanagisawa, K., and Yamaoka, H.
Subjects: Astrophysics
Abstract: We report the earliest detection of an extremely bright optical afterglow of the gamma-ray burst (GRB) 030329 using a 30cm-telescope at Tokyo Institute of Technology (Tokyo, JAPAN). Our observation started 67 minutes after the burst, and continued for succeeding two nights until the afterglow faded below the sensitivity limit of the telescope (approximately 18 mag). Combining our data with those reported in GCN Circulars, we find that the early afterglow light curve of the first half day is described by a broken power-law (t^{- alpha}) function with indices alpha_{1} = 0.88 +/- 0.01 (0.047 < t < t_{b1} days), alpha_{2} = 1.18 +/- 0.01 (t_{b1} < t < t_{b2} days), and alpha_{3} = 1.81 +/- 0.04 (t_{b2} < t < 1.2 days), where t_{b1} ~ 0.26 days and t_{b2} ~ 0.54 days, respectively. The change of the power-law index at the first break at t ~ 0.26 days is consistent with that expected from a ``cooling-break'' when the cooling frequency crossed the optical band. If the interpretation is correct, the decay index before the cooling-break implies a uniform ISM environment., Comment: 13 pages, 1 table and 2 figures. Accepted to the Astrophysical Journal Letters
Published: 2003
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25. Photospheric Abundances of Volatile and Refractory Elements in Planet-Harboring Stars

Author: Takeda, Y., Sato, B., Kambe, E., Aoki, W., Honda, S., Kawanomoto, S., Masuda, S., Izumiura, H., Watanabe, E., Koyano, H., Maehara, H., Norimoto, Y., Okada, T., Shimizu, Y., Uraguchi, F., Yanagisawa, K., Yoshida, M., Miyama, S., and Ando, H.
Subjects: Astrophysics
Abstract: By using the high-dispersion spectra of 14 bright planet-harboring stars (along with 4 reference stars) observed with the new coude echelle spectrograph at Okayama Astrophysical Observatory, we investigated the abundances of volatile elements (C, N, O, S, Zn; low condensation temperature Tc) in order to examine whether these show any significant difference compared to the abundances of other refractory elements (Si, Ti, V, Fe, Co, Ni; high Tc) which are known to be generally overabundant in those stars with planets, since a Tc-dependence is expected if the cause of such a metal-richness is due to the accretion of solid planetesimals onto the host star. We found, however, that all elements we studied behave themselves quite similarly to Fe (i.e., [X/Fe]~0) even for the case of volatile elements, which may suggest that the enhanced metallicity in those planet-bearing stars is not so much an acquired character (by accretion of rocky material) as rather primordial., Comment: 22 pages, 8 figures, to appear in PASJ
Published: 2001
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26. Infrared Star Count Models and Their Application to the Subaru Deep Field

Author: Nakajima, T., Iwamuro, F., Maihara, T., Motohara, K., Terada, H., Goto, M., Iwai, J., Tanabe, H., Taguchi, T., Hata, R., Yanagisawa, K., Iye, M., Kashikawa, N., and Tamura, M.
Subjects: Astrophysics
Abstract: We construct infrared star count models of the Galaxy applicable at faint magnitudes. In addition to dwarfs and subdwarfs, we also take into account L dwarfs, T dwarfs, and white dwarfs of both disk and halo. As a test case of the models, we analyze the infrared imaging data at J and K' obtained during the Subaru Deep Field Survey to study stellar objects. Infrared star count models we have obtained predict that the Next Generation Space Telescope will primarily see T dwarfs, M subdwarfs, and old halo white dwarfs at faint magnitudes., Comment: 20 pages, 3 figures. To be published in the November 2000 issue of the Astronomical Journal
Published: 2000
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27. PB0211 The Utilities of Multiple Genetic Analyses for Rare Coagulation Deficiencies and Rare Bleeding Disorders

Author: Uchiyama, Y., primary, Ogawa, Y., additional, Yanagisawa, K., additional, Matsumoto, A., additional, Mizuguchi, T., additional, Uchiumi, H., additional, Handa, H., additional, and Matsumoto, N., additional
Published: 2023
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28. PB0328 Outcomes of Immune-Mediated Thrombotic Thrombocytopenic Purpura at a Single Center in Japan

Author: Matsumoto, A., primary, Ogawa, Y., additional, Naito, C., additional, Yanagisawa, K., additional, Kobayashi, N., additional, Miyazawa, Y., additional, Uchiumi, H., additional, Hirakata, A., additional, Kobayashi, Y., additional, Matsumoto, M., additional, and Handa, H., additional
Published: 2023
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29. PB1233 A Single-Center Study of Reduced-Dose Corticosteroids Therapy for Patients with Acquired Hemophilia A

Author: Ogawa, Y., primary, Yanagisawa, K., additional, Matsumoto, A., additional, Kajita, M., additional, Miyazawa, Y., additional, Kobayashi, N., additional, Osaki, T., additional, Souri, M., additional, Ichinose, A., additional, and Handa, H., additional
Published: 2023
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30. Facile microwave-assisted fabrication of WC-Al2O3 composite powder from WO3-Al-C mixture

Author: BEHNAMI, A. Karimzadeh, SAKAKI, M., BAFGHI, M. Sh., and YANAGISAWA, K.
Published: 2017
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31. Low-temperature densification of Mg-doped hydroxyapatite fine powders under hydrothermal hot processing conditions

Author: Montoya-Cisneros, K.L., Rendón-Angeles, J.C., Matamoros-Veloza, Z., Matamoros-Veloza, A., and Yanagisawa, K.
Published: 2017
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32. Urea decomposition enhancing the hydrothermal synthesis of lithium iron phosphate powders: Effect of the lithium precursor

Author: Vasquez-Elizondo, L.J., Rendón-Ángeles, J.C., Matamoros-Veloza, Z., López-Cuevas, J., and Yanagisawa, K.
Published: 2017
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33. Rapid hydrothermal synthesis of SrMo1−xWxO4 powders: Structure and luminescence characterization

Author: Rendón-Angeles, J.C., Matamoros-Veloza, Z., Gonzalez, L.A., López-Cuevas, J., Ueda, T., Yanagisawa, K., Hernández-Calderón, I., and Garcia-Rocha, M.
Published: 2017
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34. Facile Preparation of SrZr1-xTixO3 and SrTi1-xZrxO3 Fine Particles Assisted by Dehydration of Zr4+ and Ti4+ Gels under Hydrothermal Conditions

Author: Quiñones-Gurrola, J. R., primary, Rendón-Angeles, J. C., additional, Matamoros-Veloza, Z., additional, López-Cuevas, J., additional, Pérez-Garibay, R., additional, and Yanagisawa, K., additional
Published: 2023
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35. Simultaneous shadowgraph imaging and acceleration pulse measurement of cavitating jet

Author: Watanabe, R., Yanagisawa, K., Yamagata, T., and Fujisawa, N.
Published: 2016
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36. Expressive visual text-to-speech as an assistive technology for individuals with autism spectrum conditions

Author: Cassidy, S.A., Stenger, B., Van Dongen, L., Yanagisawa, K., Anderson, R., Wan, V., Baron-Cohen, S., and Cipolla, R.
Published: 2016
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37. Monoiodoacetic acid induces arthritis and synovitis in rats in a dose- and time-dependent manner: proposed model-specific scoring systems

Author: Udo, M., Muneta, T., Tsuji, K., Ozeki, N., Nakagawa, Y., Ohara, T., Saito, R., Yanagisawa, K., Koga, H., and Sekiya, I.
Published: 2016
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38. Rotary-hydrothermal method assisting the conversion of celestine into scheelite SrWO4 in alkaline solutions

Author: Rendón-Angeles, J.C., Matamoros-Veloza, Z., López-Cuevas, J., Perez-Garibay, R., Diaz-Algara, J., and Yanagisawa, K.
Published: 2016
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39. Low temperature preparation of porous materials from TV panel glass compacted via hydrothermal hot pressing

Author: Matamoros-Veloza, Z., Rendón-Angeles, J.C., Yanagisawa, K., Mejia-Martínez, E.E., and Parga, J.R.
Published: 2015
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40. TTF-1/NKX2-1 binds to DDB1 and confers replication stress resistance to lung adenocarcinomas

Author: Liu, Z, Yanagisawa, K, Griesing, S, Iwai, M, Kano, K, Hotta, N, Kajino, T, Suzuki, M, and Takahashi, T
Published: 2017
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41. NIRS-Based Neurofeedback Learning Systems for Controlling Activity of the Prefrontal Cortex

Author: Sakatani, Kaoru, Takemoto, N., Tsujii, T., Yanagisawa, K., Tsunashima, H., Cohen, Irun R., Series Editor, Lajtha, Abel, Series Editor, Paoletti, Rodolfo, Series Editor, Lambris, John D., Series Editor, Van Huffel, Sabine, editor, Naulaers, Gunnar, editor, Caicedo, Alexander, editor, Bruley, Duane F., editor, and Harrison, David K., editor
Published: 2013
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42. Single-step synthesis of SrMoO4 particles from SrSO4 and their anti-corrosive activity

Author: Diaz-Algara, J., Rendón-Angeles, J.C., Matamoros-Veloza, Z., Yanagisawa, K., Rodriguez-Galicia, J.L., and Rivera-Cobo, J.M.
Published: 2014
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43. Basic mechanism of self-healing from thermal runaway for uninsulated REBCO pancake coils

Author: Yanagisawa, Y., Sato, K., Yanagisawa, K., Nakagome, H., Jin, X., Takahashi, M., and Maeda, H.
Published: 2014
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44. Synthesis of nanocrystalline TiB2 powder from TiO2, B2O3 and Mg reactants through microwave-assisted self-propagating high-temperature synthesis method

Author: GHANBARI, A, SAKAKI, M, FAEGHINIA, A, BAFGHI, M SH, and YANAGISAWA, K
Published: 2016
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45. Microelectrochemistry of dual-phase steel corroding in 0.1 M sulfuric acid

Author: Fushimi, K., Yanagisawa, K., Nakanishi, T., Hasegawa, Y., Kawano, T., and Kimura, M.
Published: 2013
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46. TEM studies of domain formation mechanisms in MnV2O4

Author: Murakami, Y., Nii, Y., Arima, T., Shindo, D., Yanagisawa, K., and Tonomura, A.
Published: 2013
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47. Determination of magnetic flux density at the nanometer-scale antiphase boundary in Heusler alloy Ni50Mn25Al12.5Ga12.5

Author: Murakami, Y., Yanagisawa, K., Niitsu, K., Park, H.S., Matsuda, T., Kainuma, R., Shindo, D., and Tonomura, A.
Published: 2013
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48. Microwave-assisted Hydrothermal Hydrolysis of Maltose with Addition of Microwave Absorbing Agents

Author: Tsubaki, S., Onda, A., Yanagisawa, K., and Azuma, J.
Published: 2012
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49. Arf tumor suppressor disrupts the oncogenic positive feedback loop including c-Myc and DDX5

Author: Tago, K, Funakoshi-Tago, M, Itoh, H, Furukawa, Y, Kikuchi, J, Kato, T, Suzuki, K, and Yanagisawa, K
Published: 2015
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50. Hydrothermal synthesis of perovskite strontium doped lanthanum chromite fine powders and its sintering

Author: Rendón-Angeles, J.C., Yanagisawa, K., Matamoros-Veloza, Z., Pech-Canul, M.I., Mendez-Nonell, J., and Torre, S. Diaz-de la
Published: 2010
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