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3,328 results on '"Ota, K."'

1. Zero-field current-induced Hall effect in ferrotoroidic metal

Author: Ota, K., Shimozawa, M., Muroya, T., Miyamoto, T., Hosoi, S., Nakamura, A., Homma, Y., Honda, F., Aoki, D., and Izawa, K.
Subjects: Condensed Matter - Strongly Correlated Electrons, Condensed Matter - Materials Science
Abstract: We have performed precise Hall measurements for the ferrotoroidic candidate material UNi4B. Below Neel temperature TN ~ 20 K (corresponding to the ferrotoroidic transition temperature), a Hall voltage becomes finite even at zero field and changes proportional to the square of current density; by contrast, it is almost zero above TN. Moreover, we have found that a current-induced magnetization estimated from our Hall effect measurements is qualitatively consistent with the previous directly measured value. These results provide strong evidence for a magnetoelectric phenomenon uniquely in ferrotoroidic metals -- a zero-field nonlinear Hall effect resulting from the current-induced magnetization connecting the ferrotoroidal moments., Comment: 6 pages, 4 figures
Published: 2022

2. A puzzling non-detection of [O III] and [C II] from a $z \approx 7.7$ galaxy observed with ALMA

Author: Binggeli, C., Inoue, A. K., Hashimoto, T., Toribio, M. C., Zackrisson, E., Ramstedt, S., Mawatari, K., Harikane, Y., Matsuo, H., Okamoto, T., Ota, K., Shimizu, I., Tamura, Y., Taniguchi, Y., and Umehata, H.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Characterizing the galaxy population in the early Universe holds the key to understanding the evolution of these objects and the role they played in cosmic reionization. However, the number of observations at the very highest redshifts are to date, few. In order to shed light on the properties of galaxies in the high-redshift Universe and their interstellar media, we observe the Lyman-$\alpha$ emitting galaxy z7\_GSD\_3811 at $z=7.664$ with band 6 and 8 at the Atacama Large Millimeter/submillimeter Array (ALMA). We target the far-infrared [O III] 88 $\mu m$, [C II] 158 $\mu m$ emission lines and dust continuum in the star-forming galaxy z7\_GSD\_3811 with ALMA. We combine these measurements with earlier observations in the rest-frame ultraviolet (UV) in order to characterize the object, and compare results to those of earlier studies observing [O III] and [C II] emission in high-redshift galaxies. The [O III] 88 $\mu m$ and [C II] 158 $\mu m$ emission lines are undetected at the position of z7\_GSD\_3811, with $3\sigma$ upper limits of $1.6 \ \times \ 10^{8} \ L_{\odot}$ and $4.0 \ \times \ 10^{7} \ L_{\odot}$, respectively. We do not detect any dust continuum in band 6 nor band 8. The measured rms in the band 8 and band 6 continuum is 26 and 9.9 $\mu Jy \ beam^{-1}$, respectively. Similar to several other high-redshift galaxies, z7\_GSD\_3811 exhibits low [C II] emission for its star formation rate compared to local galaxies. Furthermore, our upper limit on the [O III] line luminosity is lower than all the previously observed [O III] lines in high-redshift galaxies with similar ultraviolet luminosities. Our ALMA band 6 and 8 dust continuum observations imply that z7\_GSD\_3811 likely has a low dust content, and our non-detections of the [O III] and [C II] lines could indicate that z7\_GSD\_3811 has a low metallicity ($Z \lesssim 0.1 \ Z_{\odot}$)., Comment: 13 pages, 7 figures, accepted for publication in Astronomy and Astrophysics
Published: 2020
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3. Bacteremia Caused by Kalamiella piersonii Found in an Infant During the Course of Gastrointestinal Food Allergy

Author: Sada J, Hirai J, Ota K, Numoto S, Honma H, Mori N, Sakanashi D, Mikamo H, and Okumura A
Subjects: kalamiella piersonii, 16s rrna, non-ige mediated gastrointestinal food allergy, matrix-assisted laser desorption/ionization time-of-flight mass spectrometry, Infectious and parasitic diseases, RC109-216
Abstract: Jun Sada,1 Jun Hirai,2,3 Koki Ota,1 Shingo Numoto,1 Hitoshi Honma,1 Nobuaki Mori,2,3 Daisuke Sakanashi,3 Hiroshige Mikamo,2,3 Akihisa Okumura1 1Department of Pediatrics, Aichi Medical University Hospital, Nagakute, Aichi, Japan; 2Department of Clinical Infectious Diseases, Aichi Medical University Hospital, Nagakute, Aichi, Japan; 3Department of Infection Control and Prevention, Aichi Medical University Hospital, Nagakute, Aichi, JapanCorrespondence: Jun Sada, Department of Pediatrics, Aichi Medical University Hospital, 1-1, Yazako-karimata, Nagakute, Aichi, 480-1195, Japan, Tel +81-561-62-3311, Fax +81-561-76-2673, Email sada.jun.043@mail.aichi-med-u.ac.jpAbstract: Kalamiella piersonii is rare pathogen, and its pathogenicity to humans has been unknown. We describe an infant with bacteremia caused by Kalamiella piersonii. The patient was a 2-month-old girl presented with diarrhea, poor oral intake, and vomiting. The patient was tentatively diagnosed with acute enterocolitis. After admission, the patient developed a fever and blood culture yielded Gram-negative cocci, first determined to be Pantoea septica by matrix-assisted laser desorption/ionization time-of-flight mass spectrometry. However, genetic analysis of 16S rRNA allowed its identification as Kalamiella piersonii (GenBank accession number is OQ547240). Other housekeeping genes such as gyrB, rpoB, and atpD also identified the isolated strain as Kalamiella piersonii. The patient was successfully treated with cefotaxime without sequelae. Later, the patient was diagnosed as non-IgE-mediated gastrointestinal food allergy. Our experience indicated that Kalamiella piersonii is a potential human pathogen that can cause invasive infections even in infants and children. Identification of Kalamiella piersonii is difficult with routine conventional tests, and detailed studies including genetic analyses are necessary to clarify the pathogenicity of Kalamiella piersonii in humans.Keywords: Kalamiella piersonii, 16S rRNA, non-IgE-mediated gastrointestinal food allergy, matrix-assisted laser desorption/ionization time-of-flight mass spectrometry
Published: 2023

4. Discovery of Protoclusters at z ∼ 3.7 and 4.9: Embedded in Primordial Superclusters

Author: Toshikawa, J, Malkan, MA, Kashikawa, N, Overzier, R, Uchiyama, H, Ota, K, Ishikawa, S, and Ito, K
Subjects: Lyman-break galaxies, Galaxy environments, High-redshift galaxy clusters, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Astronomy & Astrophysics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We have carried out follow-up spectroscopy on three overdense regions of g- and r-dropout galaxies in the Canada-France-Hawaii Telescope Legacy Survey Deep Fields, finding two new protoclusters at z = 4.898 and 3.721 and a possible protocluster at z = 3.834. The z = 3.721 protocluster overlaps with a previously identified protocluster at z = 3.675. The redshift separation between these two protoclusters is Δz = 0.05, which is slightly larger than the size of typical protoclusters. Therefore, if they are not the progenitors of a >1015 M halo, they would grow into closely located independent halos like a supercluster. The other protocluster at z = 4.898 is also surrounded by smaller galaxy groups. These systems including protoclusters and neighboring groups are regarded as the early phase of superclusters. We quantify the spatial distribution of member galaxies of the protoclusters at z = 3.675 and 3.721 by fitting triaxial ellipsoids, finding a tentative difference: one has a pancake-like shape, while the other is filamentary. This could indicate that these two protoclusters are in different stages of formation. We investigate the relation between redshift and the velocity dispersion of protoclusters, including other protoclusters from the literature, in order to compare their dynamical states. Although there is no significant systematic trend in the velocity dispersions of protoclusters with redshift, the distribution is skewed to higher velocity dispersion over the redshift range of z = 2-6. This could be interpreted as two phases of cluster formation, one dominated by the steady accretion of galaxies and the other by the merging between group-size halos, perhaps depending on the surrounding large-scale environments.
Published: 2020

5. A pre-specified analysis of the Dapagliflozin and Prevention of Adverse Outcomes in Chronic Kidney Disease (DAPA-CKD) randomized controlled trial on the incidence of abrupt declines in kidney function

Author: Heerspink, Hiddo J.L., Wheeler, David C., Chertow, Glenn, Correa-Rotter, Ricardo, Greene, Tom, Hou, Fan Fan, McMurray, John, Rossing, Peter, Toto, Robert, Stefansson, Bergur, Langkilde, Anna Maria, Maffei, L.E., Raffaele, P., Solis, S.E., Arias, C.A., Aizenberg, D., Luquez, C., Zaidman, C., Cluigt, N., Mayer, M., Alvarisqueta, A., Wassermann, A., Maldonado, R., Bittar, J., Maurich, M., Gaite, L.E., Garcia, N., Sivak, L., Ramallo, P.O., Santos, J.C., Garcia Duran, R., Oddino, J.A., Maranon, A., Maia, L.N., Avila, D.D., Barros, E.J.G., Vidotti, M.H., Panarotto, D., Noronha, I.D.L., Turatti, L.A.A., Deboni, L., Canziani, M.E., Riella, M.C., Bacci, M.R., Paschoalin, R.P., Franco, R.J., Goldani, J.C., St-Amour, E., Steele, A.W., Goldenberg, R., Pandeya, S., Bajaj, H., Cherney, D., Kaiser, S.M., Conway, J.R., Chow, S.S., Bailey, G., Lafrance, J., Winterstein, J., Cournoyer, S., Gaudet, D., Madore, F., Houlden, R.L., Dowell, A., Langlois, M., Muirhead, N., Khandwala, H., Levin, A., Hou, F., Xue, Y., Zuo, L., Hao, C., Ni, Z., Xing, C., Chen, N., Dong, Y., Zhou, R., Xiao, X., Zou, Y., Wang, C., Liu, B., Chen, Q., Lin, M., Luo, Q., Zhang, D., Wang, J., Chen, M., Wang, X., Zhong, A., Dong, J., Zhu, C., Yan, T., Luo, P., Ren, Y., Pai, P., Li, D., Zhang, R., Zhang, J., Xu, M., Zhuang, Y., Kong, Y., Yao, X., Peng, X., Persson, F.I., Hansen, T.K., Borg, R., Pedersen Bjergaard, U., Hansen, D., Hornum, M., Haller, H., Klausmann, G., Tschope, D., Kruger, T., Gross, P., Hugo, C., Obermuller, N., Rose, L., Mertens, P., Zeller-Stefan, H., Fritsche, A., Renders, L., Muller, J., Budde, K., Schroppel, B., Wittmann, I., Voros, P., Dudas, M., Tabak, G.A., Kirschner, R., Letoha, A., Balku, I., Hermanyi, Z., Zakar, G., Mezei, I., Nagy, G.G., Lippai, J., Nemeth, A., Khullar, D., Gowdaiah, P.K., Fernando Mervin, E., Rao, V.A., Dewan, D., Goplani, K., Maddi, V.S.K., Vyawahare, M.S., Pulichikkat, R.K., Pandey, R., Sonkar, S.K., Gupta, V.K., Agarwal, S., Asirvatham, A.J., Ignatius, A., Chaubey, S., Melemadathil, S., Alva, H., Kadam, Y., Shimizu, H., Sueyoshi, A., Takeoka, H., Abe, Y., Imai, T., Onishi, Y., Fujita, Y., Tokita, Y., Oura, M., Makita, Y., Idogaki, A., Koyama, R., Kikuchi, H., Kashihara, N., Hayashi, T., Ando, Y., Tanaka, T., Shimizu, M., Hidaka, S., Gohda, T., Tamura, K., Abe, M., Kamijo, Y., Imasawa, T., Takahashi, Y., Nakayama, M., Tomita, M., Hirano, F., Fukushima, Y., Kiyosue, A., Kurioka, S., Imai, E., Kitagawa, K., Waki, M., Wada, J., Uehara, K., Iwatani, H., Ota, K., Shibazaki, S., Katayama, K., Narita, I., Iinuma, M., Matsueda, S., Sasaki, S., Yokochi, A., Tsukamoto, T., Yoshimura, T., Kang, S., Lee, S., Lim, C.S., Chin, H., Joo, K.W., Han, S.Y., Chang, T.I., Park, S., Park, H., Park, C.W., Han, B.G., Cha, D.R., Yoon, S.A., Kim, W., Kim, S.W., Ryu, D., Correa Rotter, R., Irizar Santana, S.S., Hernandez Llamas, G., Valdez Ortiz, R., Secchi Nicolas, N.C., Gonzalez Galvez, G., Lazcano Soto, J.R., Bochicchio Riccardelli, T., Bayram Llamas, E.A., Ramos Ibarra, D.R., Melo, M.G.S., Gonzalez Gonzalez, J.G., Sanchez Mijangos, J.H., Madero Robalo, M., Garcia Castillo, A., Manrique, H.A., Farfan, J.C., Vargas, R., Valdivia, A., Dextre, A., Escudero, E., Calderon Ticona, J.R., Gonzales, L., Villena, J., Leon, L., Molina, G., Saavedra, A., Garrido, E., Arbanil, H., Vargas Marquez, S., Rodriguez, J., Isidto, R., Villaflor, A.J., Gumba, M.A., Tirador, L., Comia, R.S., Sy, R.A., Guanzon, M.L.V.V., Aquitania, G., De Asis, N.C., Silva, A.A., Romero, C.M., Lim, M.E., Danguilan, R.A., Nowicki, M., Rudzki, H., Landa, K., Kucharczyk-Bauman, I., Gogola-Migdal, B., Golski, M., Olech-Cudzik, A., Stompor, T., Szczepanik, T., Miklaszewicz, B., Sciborski, R., Kuzniewski, M., Ciechanowski, K., Wronska, D., Klatko, W., Mazur, S., Popenda, G., Myslicki, M., Bolieva, L.Z., Berns, S., Galyavich, A., Abissova, T., Karpova, I., Platonov, D., Koziolova, N., Kvitkova, L., Nilk, R., Medina, T., Rebrov, A., Rossovskaya, M., Sinitsina, I., Vishneva, E., Zagidullin, N., Novikova, T., Krasnopeeva, N., Magnitskaya, O., Antropenko, N., Batiushin, M., Escudero Quesada, V., Barrios Barrea, C., Espinel Garauz, E., Cruzado Garrit, J.M., Morales Portillo, C., Gorriz Teruel, J.L., Cigarran Guldris, S., Praga Terente, M., Robles Perez-Monteoliva, N.R., Tinahones Madueno, F.J., Soto Gonzalez, A., Diaz Rodriguez, C., Furuland, H., Saeed, A., Dreja, K., Spaak, J., Bruchfeld, A., Kolesnyk, M., Levchenko, O., Pyvovarova, N., Stus, V., Doretskyy, V., Korobova, N., Horoshko, O., Katerenchuk, I., Mostovoy, Y.M., Orynchak, M., Legun, O., Dudar, I., Bilchenko, O., Andreychyn, S., Levchenko, A., Zub, L., Tereshchenko, N., Topchii, I., Ostapenko, T., Bezuglova, S., Kopytsya, M., Turenko, O., Mark, P., Barratt, J., Bhandari, S., Fraser, D., Kalra, P., Kon, S.P., Mccafferty, K., Mikhail, A., Alvarado, O.P., Anderson, R., Andrawis, N.S., Arif, A., Benjamin, S.A., Bueso, G., Busch, R.S., Carr, K.W., Crawford, P., Daboul, N., De La Calle, G.M., Delgado, B., Earl, J., El-Shahawy, M.A., Graf, R.J., Greenwood, G., Guevara, A., Wendland, E.M., Mayfield, R.K., Montero, M., Morin, D.J., Narayan, P., Numrungroad, V., Reddy, A.C., Reddy, R., Samson, M.B., Trejo, R., Butcher, M.B., Wise, J.K., Zemel, L.R., Raikhel, M., Weinstein, D., Hernandez, P., Wynne, A., Khan, B.V., Sterba, G.A., Jamal, A., Ross, D., Rovner, S.F., Tan, A., Ovalle, F., Patel, R.J., Talano, J., Patel, D.R., Burgner, A., Aslam, N., Elliott, M., Goral, S., Jovanovich, A., Manley, J.A., Umanath, K., Waguespack, D., Weiner, D., Yu, M., Schneider, L., Jalal, D., Le, T., Nguyen, N., Nguyen, H., Nguyen, D., Nguyen, V., Do, T., Chu, P., Ta, D., Tran, N., Pham, B., Pfeffer, Marc A., Pocock, Stuart, Swedberg, Karl, Rouleau, Jean L., Chaturvedi, Nishi, Ivanovich, Peter, Levey, Andrew S., Christ-Schmidt, Heidi, Held, Claes, Christersson, Christina, Mann, Johannes, Varenhorst, Christoph, Cherney, David, Postmus, Douwe, Stefánsson, Bergur V., Chertow, Glenn M., Dwyer, Jamie P., Kosiborod, Mikhail, McMurray, John J.V., Sjöström, C. David, and Toto, Robert D.
Published: 2022
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6. New Constraints on the Molecular Gas in the Prototypical HyLIRGs BRI1202-0725 & BRI1335-0417

Author: Jones, G. C., Carilli, C. L., Momjian, E., Wagg, J., Riechers, D. A., Walter, F., Decarli, R., Ota, K., and McMahon, R. G.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present Karl G Jansky Very Large Array (VLA) observations of CO(2-1) line emission and rest-frame 250GHz continuum emission of the Hyper-Luminous IR Galaxies (HyLIRGs) BRI1202-0725 (z=4.69) and BRI1335-0417 (z=4.41), with an angular resolution as high as 0.15". Our low order CO observations delineate the cool molecular gas, the fuel for star formation in the systems, in unprecedented detail. For BRI1202-0725, line emission is seen from both extreme starburst galaxies: the quasar host and the optically obscured submm galaxy (SMG), in addition to one of the Lyman-alpha emitting galaxies in the group. Line emission from the SMG shows an east-west extension of about 0.6". For Lyalpha-2, the CO emission is detected at the same velocity as [CII] and [NII], indicating a total gas mass ~4.0*10^10 solar masses. The CO emission from BRI1335-0417 peaks at the nominal quasar position, with a prominent northern extension (~1", a possible tidal feature). The gas depletion timescales are ~10^7 years for the three HyLIRGs, consistent with extreme starbursts, while that of Lyalpha-2 may be consistent with main sequence galaxies. We interpret these sources as major star formation episodes in the formation of massive galaxies and supermassive black holes (SMBHs) via gas rich mergers in the early Universe., Comment: 28 pages, 10 figures, Accepted for publication in ApJ
Published: 2016
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7. ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Search for [CII] line and dust emission in 6<z<8 galaxies

Author: Aravena, M., Decarli, R., Walter, F., Bouwens, R., Oesch, P. A., Carilli, C. L., Bauer, F. E., Da Cunha, E., Daddi, E., Gónzalez-López, J., Ivison, R. J., Riechers, D. A., Smail, Ian, Swinbank, A. M., Weiss, A., Anguita, T., Bacon, R., Bell, E., Bertoldi, F., Cortes, P., Cox, P., Hodge, J., Ibar, E., Inami, H., Infante, L., Karim, A., Magnelli, B., Ota, K., Popping, G., van der Werf, P., Wagg, J., and Fudamoto, Y.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a search for [CII] line and dust continuum emission from optical dropout galaxies at $z>6$ using ASPECS, our ALMA Spectroscopic Survey in the Hubble Ultra-Deep Field (UDF). Our observations, which cover the frequency range $212-272$ GHz, encompass approximately the range $6$4.5 $\sigma$, two of which correspond to blind detections with no optical counterparts. At this significance level, our statistical analysis shows that about 60\% of our candidates are expected to be spurious. For one of our blindly selected [CII] line candidates, we tentatively detect the CO(6-5) line in our parallel 3-mm line scan. None of the line candidates are individually detected in the 1.2 mm continuum. A stack of all [CII] candidates results in a tentative detection with $S_{1.2mm}=14\pm5\mu$Jy. This implies a dust-obscured star formation rate (SFR) of $(3\pm1)$ M$_\odot$ yr$^{-1}$. We find that the two highest--SFR objects have candidate [CII] lines with luminosities that are consistent with the low-redshift $L_{\rm [CII]}$ vs. SFR relation. The other candidates have significantly higher [CII] luminosities than expected from their UV--based SFR. At the current sensitivity it is unclear whether the majority of these sources are intrinsically bright [CII] emitters, or spurious sources. If only one of our line candidates was real (a scenario greatly favored by our statistical analysis), we find a source density for [CII] emitters at $6
Published: 2016
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8. ALMA spectroscopic survey in the Hubble Ultra Deep Field: Continuum number counts, resolved 1.2-mm extragalactic background, and properties of the faintest dusty star forming galaxies

Author: Aravena, M., Decarli, R., Walter, F., Da Cunha, E., Bauer, F. E., Carilli, C. L., Daddi, E., Elbaz, D., Ivison, R. J., Riechers, D. A., Smail, I., Swinbank, A. M., Weiss, A., Anguita, T., Assef, R. J., Bell, E., Bertoldi, F., Bacon, R., Bouwens, R., Cortes, P., Cox, P., Gónzalez-López, J., Hodge, J., Ibar, E., Inami, H., Infante, L., Karim, A., Fèvre, O. Le, Magnelli, B., Ota, K., Popping, G., Sheth, K., van der Werf, P., and Wagg, J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present an analysis of a deep (1$\sigma$=13 $\mu$Jy) cosmological 1.2-mm continuum map based on ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field. In the 1 arcmin$^2$ covered by ASPECS we detect nine sources at $>3.5\sigma$ significance at 1.2-mm. Our ALMA--selected sample has a median redshift of $z=1.6\pm0.4$, with only one galaxy detected at z$>$2 within the survey area. This value is significantly lower than that found in millimeter samples selected at a higher flux density cut-off and similar frequencies. Most galaxies have specific star formation rates similar to that of main sequence galaxies at the same epoch, and we find median values of stellar mass and star formation rates of $4.0\times10^{10}\ M_\odot$ and $\sim40~M_\odot$ yr$^{-1}$, respectively. Using the dust emission as a tracer for the ISM mass, we derive depletion times that are typically longer than 300 Myr, and we find molecular gas fractions ranging from $\sim$0.1 to 1.0. As noted by previous studies, these values are lower than using CO--based ISM estimates by a factor $\sim$2. The 1\,mm number counts (corrected for fidelity and completeness) are in agreement with previous studies that were typically restricted to brighter sources. With our individual detections only, we recover $55\pm4\%$ of the extragalactic background light (EBL) at 1.2 mm measured by the Planck satellite, and we recover $80\pm7\%$ of this EBL if we include the bright end of the number counts and additional detections from stacking. The stacked contribution is dominated by galaxies at $z\sim1-2$, with stellar masses of (1-3)$\times$10$^{10}$ M$_\odot$. For the first time, we are able to characterize the population of galaxies that dominate the EBL at 1.2 mm., Comment: Accepted for publication on the Astrophysical Journal
Published: 2016
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9. ALMA constraints on the faint millimetre source number counts and their contribution to the cosmic infrared background

Author: Carniani, S., Maiolino, R., De Zotti, G., Negrello, M., Marconi, A., Bothwell, M. S., Capak, P., Carilli, C., Castellano, M., Cristiani, S., Ferrara, A., Fontana, A., Gallerani, S., Jones, G., Ohta, K., Ota, K., Pentericci, L., Santini, P., Sheth, K., Vallini, L., Vanzella, E., Wagg, J., and Williams, R. J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have analysed 18 ALMA continuum maps in Bands 6 and 7, with rms down to 7.8$\mu$Jy, to derive differential number counts down to 60$\mu$Jy and 100$\mu$Jy at $\lambda=$1.3 mm and $\lambda=$1.1 mm, respectively. The area covered by the combined fields is $\rm 9.5\times10^{-4}deg^2$ at 1.1mm and $\rm 6.6\times10^{-4}deg^{2}$ at 1.3mm. We improved the source extraction method by requiring that the dimension of the detected sources be consistent with the beam size. This method enabled us to remove spurious detections that have plagued the purity of the catalogues in previous studies. We detected 50 faint sources with S/N$>$3.5 down to 60$\mu$Jy, hence improving the statistics by a factor of four relative to previous studies. The inferred differential number counts are $\rm dN/d(Log_{10}S)=1\times10^5~deg^2$ at a 1.1 mm flux $S_{\lambda = 1.1~mm} = 130~\mu$Jy, and $\rm dN/d(Log_{10}S)=1.1\times10^5~deg^2$ at a 1.3 mm flux $\rm S_{\lambda = 1.3~mm} = 60~\mu$Jy. At the faintest flux limits, i.e. 30$\mu$Jy and 40$\mu$Jy, we obtain upper limits on the differential number counts of $\rm dN/d(Log_{10}S) < 7\times10^5~deg^2$ and $\rm dN/d(Log_{10}S)<3\times10^5~deg^2$, respectively. Our results provide a new lower limit to CIB intensity of 17.2${\rm Jy\ deg^{-2}}$ at 1.1mm and of 12.9${\rm Jy\ deg^{-2}}$ at 1.3mm. Moreover, the flattening of the integrated number counts at faint fluxes strongly suggests that we are probably close to the CIB intensity. Our data imply that galaxies with SFR$<40~M_{\odot}/yr$ certainly contribute less than 50% to the CIB while more than 50% of the CIB must be produced by galaxies with $\rm SFR>40~M_{\odot}/yr$. The differential number counts are in nice agreement with recent semi-analytical models of galaxy formation even as low as our faint fluxes. Consequently, this supports the galaxy evolutionary scenarios and assumptions made in these models., Comment: 11 pages, 9 figures, A&A accepted
Published: 2015
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10. A SYSTEMATIC SURVEY of PROTOCLUSTERS at z ∼ 3-6 in the CFHTLS DEEP FIELDS

Author: Toshikawa, J, Kashikawa, N, Overzier, R, Malkan, MA, Furusawa, H, Ishikawa, S, Onoue, M, Ota, K, Tanaka, M, Niino, Y, and Uchiyama, H
Subjects: early universe, galaxies: clusters: general, galaxies: high-redshift, large-scale structure of universe, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We present the discovery of three protoclusters at z ∼ 3-4 with spectroscopic confirmation in the Canada-France-Hawaii Telescope Legacy Survey Deep Fields. In these fields, we investigate the large-scale projected sky distribution of z ∼ 3-6 Lyman-break galaxies and identify 21 protocluster candidates from regions that are overdense at more than 4σ overdensity significance. Based on cosmological simulations, it is expected that more than 76% of these candidates will evolve into a galaxy cluster of at least a halo mass of 1014 M o at z = 0. We perform follow-up spectroscopy for eight of the candidates using Subaru/FOCAS, Keck II/DEIMOS, and Gemini-N/GMOS. In total we target 462 dropout candidates and obtain 138 spectroscopic redshifts. We confirm three real protoclusters at z = 3-4 with more than five members spectroscopically identified and find one to be an incidental overdense region by mere chance alignment. The other four candidate regions at z ∼ 5-6 require more spectroscopic follow-up in order to be conclusive. A z = 3.67 protocluster, which has 11 spectroscopically confirmed members, shows a remarkable core-like structure composed of a central small region (
Published: 2016

11. The spectral energy distribution of the redshift 7.1 quasar ULAS J1120+0641

Author: Barnett, R., Warren, S. J., Banerji, M., McMahon, R. G., Hewett, P. C., Mortlock, D. J., Simpson, C., Venemans, B. P., Ota, K., and Shibuya, T.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present new observations of the highest-redshift quasar known, ULAS J1120+0641, redshift $z=7.084$, obtained in the optical, at near-, mid-, and far-infrared wavelengths, and in the sub-mm. We combine these results with published X-ray and radio observations to create the multiwavelength spectral energy distribution (SED), with the goals of measuring the bolometric luminosity $L_{\rm bol}$, and quantifying the respective contributions from the AGN and star formation. We find three components are needed to fit the data over the wavelength range $0.12-1000\,\mu$m: the unobscured quasar accretion disk and broad-line region, a dusty clumpy AGN torus, and a cool 47K modified black body to characterise star formation. Despite the low signal-to-noise ratio of the new long-wavelength data, the normalisation of any dusty torus model is constrained within $\pm40\%$. We measure a bolometric luminosity $L_{\rm bol}=2.6\pm0.6\times10^{47}\,$erg$\,$s$^{-1}=6.7 \pm 1.6\times10^{13}L_{\odot}$, to which the three components contribute $31\%,32\%,3\%$, respectively, with the remainder provided by the extreme UV $<0.12\,\mu$m. We tabulate the best-fit model SED. We use local scaling relations to estimate a star formation rate (SFR) in the range $60-270\,{\rm M}_\odot$/yr from the [C$\,{\scriptsize \rm II}$] line luminosity and the $158\,\mu$m continuum luminosity. An analysis of the equivalent widths of the [C$\,{\scriptsize \rm II}$] line in a sample of $z>5.7$ quasars suggests that these indicators are promising tools for estimating the SFR in high-redshift quasars in general. At the time observed the black hole was growing in mass more than 100 times faster than the stellar bulge, relative to the mass ratio measured in the local universe, i.e. compared to ${M_{\rm BH}}/{M_{\rm bulge}} \simeq 1.4\times10^{-3}$, for ULAS J1120+0641 we measure ${\dot{M}_{\rm BH}}/{\dot{M}_{\rm bulge}} \simeq 0.2$., Comment: Accepted for publication in A&A. 10 pages, 5 figures, 5 tables
Published: 2014
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12. The Use of the Japanese Public Financial Support Has Positive Impact on Persistence with Outpatient Treatments for Schizophrenia: Single-center Retrospective Cohort Study in Japan

Author: Arikawa M, Ota K, Azekawa T, Ohashi S, Funaoka Y, Yoshiie H, Koshi H, Takaishi Y, and Nakao S
Subjects: schizophrenia, treatment persistence, financial support, jiritsu-shien-iryo-hi, Medicine (General), R5-920
Abstract: Masatoshi Arikawa,1 Kazumi Ota,2 Takaharu Azekawa,1 Shizuko Ohashi,1 Yoichi Funaoka,1 Hiroshi Yoshiie,1 Haruka Koshi,1 Yohei Takaishi,1 Saeka Nakao1 1Department of Psychiatry, Shioiri Mental Clinic, Yokosuka, Kanagawa, Japan; 2Department of Psychiatry, Juntendo University School of Medicine, Tokyo, JapanCorrespondence: Masatoshi ArikawaDepartment of Psychiatry, Shioiri Mental Clinic, Yokosuka, Kanagawa, JapanEmail masatoshi.arikawa@gmail.comPurpose: One of the challenges of treating schizophrenia is how to improve persistence with outpatient treatments. Lengthening community life by improving persistence and preventing relapse and rehospitalization can have positive influence on the patients’ personal recovery and well-being. In Japan, there is “Medical Expenses for Services and Supports for Persons with Disabilities” (“Jiritsu-shien-iryo-hi” in Japanese) which is the public financial support system for psychiatric outpatient treatments. However, it is not clear how this financial support affects persistence with outpatient treatments for patients with schizophrenia. The purpose of the study is to investigate how the financial support affects persistence with outpatient treatments for schizophrenia.Patients and Methods: Data of outpatients who visited the clinic between October 1, 2006 and September 30, 2016 was collected. The variables for the analysis were continuation and discontinuation of treatment of those who used the financial support (user) and those who did not (nonuser). The covariates were sex, age, time from onset of the disease to first visit to the clinic, number of hospitalizations in the past, use of psychiatric day care, and use of psychiatric home nursing care. Kaplan–Meier analysis was performed using propensity score matching. The observation period was five years from the first visit to the clinic.Results: Among 1155 patients who were diagnosed with schizophrenia, 718 were excluded, based on the exclusion criteria. The propensity score matching was performed for 437 patients, and the subjects for the final analysis were 278. Average survival period was 1.09 (SD ± 1.66) years for nonuser, 3.02 (SD ± 1.77) years for users, and users exhibited a significantly longer number of years of outpatient treatments (P< 0.001).Conclusion: The results indicated that use of the financial support can contribute to persistence with outpatient treatments.Keywords: schizophrenia, treatment persistence, financial support, jiritsu-shien-iryo-hi
Published: 2021

13. Initial Results from the Nobeyama Molecular Gas Observations of Distant Bright Galaxies

Author: Iono, D., Hatsukade, B., Kohno, K., Kawabe, R., Ikarashi, S., Ichikawa, K., Kodama, T., Motohara, K., Nakajima, T., Nakanishi, K., Ohta, K., Ota, K., Saito, T., Suzuki, K., Tadaki, K., Tamura, Y., Ueda, J., Umehata, H., Yabe, K., Yoshida, T., Yuma, S., Kuno, N., Takano, S., Iwashita, H., Handa, K., Higuchi, A., Hirota, A., Ishikawa, S., Kimura, K., Maekawa, J., Mikoshiba, H., Miyazawa, C., Miyazawa, K., Muraoka, K., Ogawa, H., Onodera, S., Saito, Y., Sakai, T., Takahashi, S., and Yun, M. S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present initial results from the CO survey toward high redshift galaxies using the Nobeyama 45m telescope. Using the new wide bandwidth spectrometer equipped with a two-beam SIS receiver, we have robust new detections of three high redshift (z=1.6-3.4) submillimeter galaxies (SXDF 1100.001, SDP9, and SDP17), one tentative detection (SDSS J160705+533558), and one non-detection (COSMOS-AzTEC1). The galaxies observed during the commissioning phase are sources with known spectroscopic redshifts from previous optical or from wide-band submm spectroscopy. The derived molecular gas mass and line widths from Gaussian fits are ~10^11 Msun and 430-530 km/s, which are consistent with previous CO observations of distant submm galaxies and quasars. The spectrometer that allows a maximum of 32 GHz instantaneous bandwidth will provide new science capabilities at the Nobeyama 45m telescope, allowing us to determine redshifts of bright submm selected galaxies without any prior redshift information., Comment: 4 pages, 1 figure, PASJ Letter Accepted
Published: 2012
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14. Weaning from mechanical ventilation in intensive care units across 50 countries (WEAN SAFE): a multicentre, prospective, observational cohort study

Author: Pham, T, Heunks, L, Bellani, G, Madotto, F, Aragao, I, Beduneau, G, Goligher, E, Grasselli, G, Laake, J, Mancebo, J, Penuelas, O, Piquilloud, L, Pesenti, A, Wunsch, H, van Haren, F, Brochard, L, Laffey, J, Abrough, F, Acharya, S, Amin, P, Arabi, Y, Bauer, P, Beitler, J, Berkius, J, Bugedo, G, Camporota, L, Cerny, V, Cho, Y, Clarkson, K, Estenssoro, E, Gritsan, A, Hashemian, S, Hermans, G, Jovanovic, B, Kurahashi, K, Matamis, D, Moerer, O, Molnar, Z, Ozyilmaz, E, Panka, B, Papali, A, Perbet, S, Qiu, H, Razek, A, Rittayamai, N, Roldan, R, Serpa Neto, A, Szuldrzynski, K, Talmor, D, Tomescu, D, Villagomez, A, Zeggwagh, A, Abe, T, Aboshady, A, Acampo-de Jong, M, Adderley, J, Adiguzel, N, Agrawal, V, Aguilar, G, Aguirre, G, Aguirre-Bermeo, H, Ahlstrom, B, Akbas, T, Akker, M, Al Sadeh, G, Alamri, S, Algaba, A, Ali, M, Aliberti, A, Allegue, J, Alvarez, D, Amador, J, Andersen, F, Ansari, S, Apichatbutr, Y, Apostolopoulou, O, Arellano, D, Arica, M, Arikan, H, Arinaga, K, Arnal, J, Asano, K, Asin-Corrochano, M, Avalos Cabrera, J, Avila Fuentes, S, Aydemir, S, Aygencel, G, Azevedo, L, Bacakoglu, F, Badie, J, Baedorf Kassis, E, Bai, G, Balaraj, G, Ballico, B, Banner-Goodspeed, V, Banwarie, P, Barbieri, R, Baronia, A, Barrett, J, Barrot, L, Barrueco-Francioni, J, Barry, J, Bawangade, H, Beavis, S, Beck, E, Beehre, N, Belenguer Muncharaz, A, Belliato, M, Bellissima, A, Beltramelli, R, Ben Souissi, A, Benitez-Cano, A, Benlamin, M, Benslama, A, Bento, L, Benvenuti, D, Bernabe, L, Bersten, A, Berta, G, Bertini, P, Bertram-Ralph, E, Besbes, M, Bettini, L, Beuret, P, Bewley, J, Bezzi, M, Bhakhtiani, L, Bhandary, R, Bhowmick, K, Bihari, S, Bissett, B, Blythe, D, Bocher, S, Boedjawan, N, Bojanowski, C, Boni, E, Boraso, S, Borelli, M, Borello, S, Borislavova, M, Bosma, K, Bottiroli, M, Boyd, O, Bozbay, S, Briva, A, Bruel, C, Bruni, A, Buehner, U, Bulpa, P, Burt, K, Buscot, M, Buttera, S, Cabrera, J, Caccese, R, Caironi, P, Canchos Gutierrez, I, Canedo, N, Cani, A, Cappellini, I, Carazo, J, Cardonnet, L, Carpio, D, Carriedo, D, Carrillo, R, Carvalho, J, Caser, E, Castelli, A, Castillo Quintero, M, Castro, H, Catorze, N, Cengiz, M, Cereijo, E, Ceunen, H, Chaintoutis, C, Chang, Y, Chaparro, G, Chapman, C, Chau, S, Chavez, C, Chelazzi, C, Chelly, J, Chemouni, F, Chen, K, Chena, A, Chiarandini, P, Chilton, P, Chiumello, D, Chou-Lie, Y, Chudeau, N, Cinel, I, Cinnella, G, Clark, M, Clark, T, Clementi, S, Coaguila, L, Codecido, A, Collins, A, Colombo, R, Conde, J, Consales, G, Cook, T, Coppadoro, A, Cornejo, R, Cortegiani, A, Coxo, C, Cracchiolo, A, Crespo Ramirez, M, Crova, P, Cruz, J, Cubattoli, L, Cukurova, Z, Curto, F, Czempik, P, D'Andrea, R, da Silva Ramos, F, Dangers, L, Danguy des Deserts, M, Danin, P, Dantas, F, Daubin, C, Dawei, W, de Haro, C, de Jesus Montelongo, F, De Mendoza, D, de Pablo, R, De Pascale, G, De Rosa, S, Decavele, M, Declercq, P, Deicas, A, del Carmen Campos Moreno, M, Dellamonica, J, Delmas, B, Demirkiran, O, Demirkiran, H, Dendane, T, di Mussi, R, Diakaki, C, Diaz, A, Diaz, W, Dikmen, Y, Dimoula, A, Doble, P, Doha, N, Domingos, G, Dres, M, Dries, D, Duggal, A, Duke, G, Dunts, P, Dybwik, K, Dykyy, M, Eckert, P, Efe, S, Elatrous, S, Elay, G, Elmaryul, A, Elsaadany, M, Elsayed, H, Elsayed, S, Emery, M, Ena, S, Eng, K, Englert, J, Erdogan, E, Ergin Ozcan, P, Eroglu, E, Escobar, M, Esen, F, Esen Tekeli, A, Esquivel, A, Esquivel Gallegos, H, Ezzouine, H, Facchini, A, Faheem, M, Fanelli, V, Farina, M, Fartoukh, M, Fehrle, L, Feng, F, Feng, Y, Fernandez, I, Fernandez, B, Fernandez-Rodriguez, M, Ferrando, C, Ferreira da Silva, M, Ferreruela, M, Ferrier, J, Flamm Zamorano, M, Flood, L, Floris, L, Fluckiger, M, Forteza, C, Fortunato, A, Frans, E, Frattari, A, Fredes, S, Frenzel, T, Fumagalli, R, Furche, M, Fusari, M, Fysh, E, Galeas-Lopez, J, Galerneau, L, Garcia, A, Garcia, M, Garcia, E, Garcia Olivares, P, Garlicki, J, Garnero, A, Garofalo, E, Gautam, P, Gazenkampf, A, Gelinotte, S, Gelormini, D, Ghrenassia, E, Giacomucci, A, Giannoni, R, Gigante, A, Glober, N, Gnesin, P, Gollo, Y, Gomaa, D, Gomero Paredes, R, Gomes, R, Gomez, R, Gomez, O, Gomez, A, Gondim, L, Gonzalez, M, Gonzalez, I, Gonzalez-Castro, A, Gordillo Romero, O, Gordo, F, Gouin, P, Graf Santos, J, Grainne, R, Grando, M, Granov Grabovica, S, Grasso, S, Grasso, R, Grimmer, L, Grissom, C, Gu, Q, Guan, X, Guarracino, F, Guasch, N, Guatteri, L, Gueret, R, Guerin, C, Guerot, E, Guitard, P, Gul, F, Gumus, A, Gurjar, M, Gutierrez, P, Hachimi, A, Hadzibegovic, A, Hagan, S, Hammel, C, Han Song, J, Hanlon, G, Heines, S, Henriksson, J, Herbrecht, J, Heredia Orbegoso, G, Hermon, A, Hernandez, R, Hernandez, C, Herrera, L, Herrera-Gutierrez, M, Hidalgo, J, Hill, D, Holmquist, D, Homez, M, Hongtao, X, Hormis, A, Horner, D, Hornos, M, Hou, M, House, S, Housni, B, Hugill, K, Humphreys, S, Humbert, L, Hunter, S, Hwa Young, L, Iezzi, N, Ilutovich, S, Inal, V, Innes, R, Ioannides, P, Iotti, G, Ippolito, M, Irie, H, Iriyama, H, Itagaki, T, Izura, J, Izza, S, Jabeen, R, Jamaati, H, Jamadarkhana, S, Jamoussi, A, Jankowski, M, Jaramillo, L, Jeon, K, Jeong Lee, S, Jeswani, D, Jha, S, Jiang, L, Jing, C, Jochmans, S, Johnstad, B, Jongmin, L, Joret, A, Junhasavasdikul, D, Jurado, M, Kam, E, Kamohara, H, Kane, C, Kara, I, Karakurt, S, Karnjanarachata, C, Kataoka, J, Katayama, S, Kaushik, S, Kelebek Girgin, N, Kerr, K, Kerslake, I, Khairnar, P, Khalid, A, Khan, A, Khanna, A, Khorasanee, R, Kienhorst, D, Kirakli, C, Knafelj, R, Kol, M, Kongpolprom, N, Kopitko, C, Korkmaz Ekren, P, Kubisz-Pudelko, A, Kulcsar, Z, Kumasawa, J, Kuriyama, A, Kutchak, F, Labarca, E, Labat, F, Laborda, C, Laca Barrera, M, Lagache, L, Landaverde Lopez, A, Lanspa, M, Lascari, V, Le Meur, M, Lee, S, Lee, Y, Lee, J, Lee, W, Legernaes, T, Leiner, T, Lemiale, V, Leonor, T, Lepper, P, Li, D, Li, H, Li, O, Lima, A, Lind, D, Litton, E, Liu, N, Liu, L, Liu, J, Llitjos, J, Llorente, B, Lopez, R, Lopez, C, Lopez Nava, C, Lovazzano, P, Lu, M, Lucchese, F, Lugano, M, Lugo Goytia, G, Luo, H, Lynch, C, Macheda, S, Madrigal Robles, V, Maggiore, S, Magret Iglesias, M, Malaga, P, Mallapura Maheswarappa, H, Malpartida, G, Malyarchikov, A, Mansson, H, Manzano, A, Marey, I, Marin, N, Marin, M, Markman, E, Martin, F, Martin, A, Martin Dal Gesso, C, Martinez, F, Martinez-Fidalgo, C, Martin-Loeches, I, Mas, A, Masaaki, S, Maseda, E, Massa, E, Mattsson, A, Maugeri, J, Mccredie, V, Mccullough, J, Mcguinness, S, Mckown, A, Medve, L, Mei, C, Mellado Artigas, R, Mendes, V, Mervat, M, Michaux, I, Mikhaeil, M, Milagros, O, Milet, I, Millan, M, Minwei, Z, Mirabella, L, Mishra, S, Mistraletti, G, Mochizuki, K, Moghal, A, Mojoli, F, Molin, A, Montiel, R, Montini, L, Monza, G, Mora Aznar, M, Morakul, S, Morales, M, Moreno Torres, D, Morocho Tutillo, D, Motherway, C, Mouhssine, D, Mouloudi, E, Munoz, T, Munoz de Cabo, C, Mustafa, M, Muthuchellappan, R, Muthukrishnan, M, Muttini, S, Nagata, I, Nahar, D, Nakanishi, M, Nakayama, I, Namendys-Silva, S, Nanchal, R, Nandakumar, S, Nasi, A, Nasir, K, Navalesi, P, Naz Aslam, T, Nga Phan, T, Nichol, A, Niiyama, S, Nikolakopoulou, S, Nikolic, E, Nitta, K, Noc, M, Nonas, S, Nseir, S, Nur Soyturk, A, Obata, Y, Oeckler, R, Oguchi, M, Ohshimo, S, Oikonomou, M, Ojados, A, Oliveira, M, Oliveira Filho, W, Oliveri, C, Olmos, A, Omura, K, Orlandi, M, Orsenigo, F, Ortiz-Ruiz De Gordoa, L, Ota, K, Ovalle Olmos, R, Oveges, N, Oziemski, P, Ozkan Kuscu, O, Pachas Alvarado, F, Pagella, G, Palaniswamy, V, Palazon Sanchez, E, Palmese, S, Pan, G, Pan, W, Papanikolaou, M, Papavasilopoulou, T, Parekh, A, Parke, R, Parrilla, F, Parrilla, D, Pasha, T, Pasin, L, Patao, L, Patel, M, Patel, G, Pati, B, Patil, J, Pattnaik, S, Paul, D, Pavesi, M, Pavlotsky, V, Paz, G, Paz, E, Pecci, E, Pellegrini, C, Pena Padilla, A, Perchiazzi, G, Pereira, T, Pereira, V, Perez, M, Perez Calvo, C, Perez Cheng, M, Perez Maita, R, Perez-Araos, R, Perez-Teran, P, Perez-Torres, D, Perkins, G, Persona, P, Petnak, T, Petrova, M, Philippart, F, Picetti, E, Pierucci, E, Piervincenzi, E, Pinciroli, R, Pintado, M, Piraino, T, Piras, S, Piras, C, Pirompanich, P, Pisani, L, Platas, E, Plotnikow, G, Porras, W, Porta, V, Portilla, M, Portugal, J, Povoa, P, Prat, G, Pratto, R, Preda, G, Prieto, I, Prol-Silva, E, Pugh, R, Qi, Y, Qian, C, Qin, T, Qu, H, Quintana, T, Quispe Sierra, R, Quispe Soto, R, Rabbani, R, Rabee, M, Rabie, A, Rahe Pereira, M, Rai, A, Raj Ashok, S, Rajab, M, Ramdhani, N, Ramey, E, Ranieri, M, Rathod, D, Ray, B, Redwanul Huq, S, Regli, A, Reina, R, Resano Sarmiento, N, Reynaud, F, Rialp, G, Ricart, P, Rice, T, Richardson, A, Rieder, M, Rinket, M, Rios, F, Risso Vazquez, A, Riva, I, Rivette, M, Roca, O, Roche-Campo, F, Rodriguez, C, Rodriguez, G, Rodriguez Gonzalez, D, Rodriguez Tucto, X, Rogers, A, Romano, M, Rortveit, L, Rose, A, Roux, D, Rouze, A, Rubatto Birri, P, Ruilan, W, Ruiz Robledo, A, Ruiz-Aguilar, A, Sadahiro, T, Saez, I, Sagardia, J, Saha, R, Saiphoklang, N, Saito, S, Salem, M, Sales, G, Salgado, P, Samavedam, S, Sami Mebazaa, M, Samuelsson, L, San Juan Roman, N, Sanchez, P, Sanchez-Ballesteros, J, Sandoval, Y, Sani, E, Santos, M, Santos, C, Sanui, M, Saravanabavan, L, Sari, S, Sarkany, A, Sauneuf, B, Savioli, M, Sazak, H, Scano, R, Schneider, F, Schortgen, F, Schultz, M, Schwarz, G, Seckin Yucesoy, F, Seely, A, Seiler, F, Seker Tekdos, Y, Seok Chan, K, Serano, L, Serednicki, W, Setten, M, Shah, A, Shah, B, Shang, Y, Shanmugasundaram, P, Shapovalov, K, Shebl, E, Shiga, T, Shime, N, Shin, P, Short, J, Shuhua, C, Siddiqui, S, Silesky Jimenez, J, Silva, D, Silva Sales, B, Simons, K, Sjobo, B, Slessor, D, Smiechowicz, J, Smischney, N, Smith, P, Smith, T, Smith, M, Snape, S, Snyman, L, Soetens, F, Sook Hong, K, Sosa Medellin, M, Soto, G, Souloy, X, Sousa, E, Sovatzis, S, Sozutek, D, Spadaro, S, Spagnoli, M, Spangfors, M, Spittle, N, Spivey, M, Stapleton, A, Stefanovic, B, Stephenson, L, Stevenson, E, Strand, K, Strano, M, Straus, S, Sun, C, Sun, R, Sundaram, V, Sunpark, T, Surlemont, E, Sutherasan, Y, Szabo, Z, Tainter, C, Takaba, A, Tallott, M, Tamasato, T, Tang, Z, Tangsujaritvijit, V, Taniguchi, L, Taniguchi, D, Tarantino, F, Teerapuncharoen, K, Temprano, S, Terragni, P, Terzi, N, Thakur, A, Theerawit, P, Thille, A, Thomas, M, Thungtitigul, P, Thyrault, M, Tilouch, N, Timenetsky, K, Tirapu, J, Todeschini, M, Tomas, R, Tomaszewski, C, Tonetti, T, Tonnelier, A, Trinder, J, Trongtrakul, K, Truwit, J, Tsuei, B, Tulaimat, A, Turan, S, Turkoglu, M, Tyagi, S, Ubeda, A, Vagginelli, F, Valenti, M, Vallverdu, I, Van Axel, A, van den Hul, I, van der Hoeven, H, Van Der Meer, N, Vanhoof, M, Vargas-Ordonez, M, Vaschetto, R, Vascotto, E, Vatsik, M, Vaz, A, Vazquez-Sanchez, A, Ventura, S, Vermeijden, J, Vidal, A, Vieira, J, Vilela Costa Pinto, B, Villagra, A, Villegas Succar, C, Vinorum, O, Vitale, G, Vj, R, Vochin, A, Voiriot, G, Volta, C, von Seth, M, Wajdi, M, Walsh, D, Wang, S, Wardi, G, Ween-Velken, N, Wei, B, Weller, D, Welsh, D, Welters, I, Wert, M, Whiteley, S, Wilby, E, Williams, E, Williams, K, Wilson, A, Wojtas, J, Won Huh, J, Wrathall, D, Wright, C, Wu, J, Xi, G, Xing, Z, Xu, H, Yamamoto, K, Yan, J, Yanez, J, Yang, X, Yates, E, Yazicioglu Mocin, O, Ye, Z, Yildirim, F, Yoshida, N, Yoshido, H, Young Lee, B, Yu, R, Yu, G, Yu, T, Yuan, B, Yuangtrakul, N, Yumoto, T, Yun, X, Zakalik, G, Zaki, A, Zalba-Etayo, B, Zambon, M, Zang, B, Zani, G, Zarka, J, Zerbi, S, Zerman, A, Zetterquist, H, Zhang, J, Zhang, H, Zhang, W, Zhang, G, Zhao, H, Zheng, J, Zhu, B, Zumaran, R, Pham T., Heunks L., Bellani G., Madotto F., Aragao I., Beduneau G., Goligher E. C., Grasselli G., Laake J. H., Mancebo J., Penuelas O., Piquilloud L., Pesenti A., Wunsch H., van Haren F., Brochard L., Laffey J. G., Abrough F., Acharya S. P., Amin P., Arabi Y., Bauer P., Beitler J., Berkius J., Bugedo G., Camporota L., Cerny V., Cho Y. -J., Clarkson K., Estenssoro E., Goligher E., Gritsan A., Hashemian S. M., Hermans G., Heunks L. M., Jovanovic B., Kurahashi K., Matamis D., Moerer O., Molnar Z., Ozyilmaz E., Panka B., Papali A., Perbet S., Qiu H., Razek A. A., Rittayamai N., Roldan R., Serpa Neto A., Szuldrzynski K., Talmor D., Tomescu D., Villagomez A., Zeggwagh A. A., Abe T., Aboshady A., Acampo-de Jong M., Acharya S., Adderley J., Adiguzel N., Agrawal V. K., Aguilar G., Aguirre G., Aguirre-Bermeo H., Ahlstrom B., Akbas T., Akker M., Al Sadeh G., Alamri S., Algaba A., Ali M., Aliberti A., Allegue J. M., Alvarez D., Amador J., Andersen F. H., Ansari S., Apichatbutr Y., Apostolopoulou O., Arellano D., Arica M., Arikan H., Arinaga K., Arnal J. -M., Asano K., Asin-Corrochano M., Avalos Cabrera J. M., Avila Fuentes S., Aydemir S., Aygencel G., Azevedo L., Bacakoglu F., Badie J., Baedorf Kassis E., Bai G., Balaraj G., Ballico B., Banner-Goodspeed V., Banwarie P., Barbieri R., Baronia A., Barrett J., Barrot L., Barrueco-Francioni J. E., Barry J., Bawangade H., Beavis S., Beck E., Beehre N., Belenguer Muncharaz A., Belliato M., Bellissima A., Beltramelli R., Ben Souissi A., Benitez-Cano A., Benlamin M., Benslama A., Bento L., Benvenuti D., Bernabe L., Bersten A., Berta G., Bertini P., Bertram-Ralph E., Besbes M., Bettini L. R., Beuret P., Bewley J., Bezzi M., Bhakhtiani L., Bhandary R., Bhowmick K., Bihari S., Bissett B., Blythe D., Bocher S., Boedjawan N., Bojanowski C. M., Boni E., Boraso S., Borelli M., Borello S., Borislavova M., Bosma K. J., Bottiroli M., Boyd O., Bozbay S., Briva A., Bruel C., Bruni A., Buehner U., Bulpa P., Burt K., Buscot M., Buttera S., Cabrera J., Caccese R., Caironi P., Canchos Gutierrez I., Canedo N., Cani A., Cappellini I., Carazo J., Cardonnet L. P., Carpio D., Carriedo D., Carrillo R., Carvalho J., Caser E., Castelli A., Castillo Quintero M., Castro H., Catorze N., Cengiz M., Cereijo E., Ceunen H., Chaintoutis C., Chang Y., Chaparro G., Chapman C., Chau S., Chavez C. E., Chelazzi C., Chelly J., Chemouni F., Chen K., Chena A., Chiarandini P., Chilton P., Chiumello D., Chou-Lie Y., Chudeau N., Cinel I., Cinnella G., Clark M., Clark T., Clementi S., Coaguila L., Codecido A. J., Collins A., Colombo R., Conde J., Consales G., Cook T., Coppadoro A., Cornejo R., Cortegiani A., Coxo C., Cracchiolo A. N., Crespo Ramirez M., Crova P., Cruz J., Cubattoli L., Cukurova Z., Curto F., Czempik P., D'Andrea R., da Silva Ramos F., Dangers L., Danguy des Deserts M., Danin P. -E., Dantas F., Daubin C., Dawei W., de Haro C., de Jesus Montelongo F., De Mendoza D., de Pablo R., De Pascale G., De Rosa S., Decavele M., Declercq P. -L., Deicas A., del Carmen Campos Moreno M., Dellamonica J., Delmas B., Demirkiran O., Demirkiran H., Dendane T., di Mussi R., Diakaki C., Diaz A., Diaz W., Dikmen Y., Dimoula A., Doble P., Doha N., Domingos G., Dres M., Dries D., Duggal A., Duke G., Dunts P., Dybwik K., Dykyy M., Eckert P., Efe S., Elatrous S., Elay G., Elmaryul A. S., Elsaadany M., Elsayed H., Elsayed S., Emery M., Ena S., Eng K., Englert J. A., Erdogan E., Ergin Ozcan P., Eroglu E., Escobar M., Esen F., Esen Tekeli A., Esquivel A., Esquivel Gallegos H., Ezzouine H., Facchini A., Faheem M., Fanelli V., Farina M. F., Fartoukh M., Fehrle L., Feng F., Feng Y., Fernandez I., Fernandez B., Fernandez-Rodriguez M. L., Ferrando C., Ferreira da Silva M. J., Ferreruela M., Ferrier J., Flamm Zamorano M. J., Flood L., Floris L., Fluckiger M., Forteza C., Fortunato A., Frans E., Frattari A., Fredes S., Frenzel T., Fumagalli R., Furche M. A., Fusari M., Fysh E., Galeas-Lopez J. L., Galerneau L. -M., Garcia A., Garcia M. F., Garcia E., Garcia Olivares P., Garlicki J., Garnero A., Garofalo E., Gautam P., Gazenkampf A., Gelinotte S., Gelormini D., Ghrenassia E., Giacomucci A., Giannoni R., Gigante A., Glober N., Gnesin P., Gollo Y., Gomaa D., Gomero Paredes R., Gomes R., Gomez R. A., Gomez O., Gomez A., Gondim L., Gonzalez M., Gonzalez I., Gonzalez-Castro A., Gordillo Romero O., Gordo F., Gouin P., Graf Santos J., Grainne R., Grando M., Granov Grabovica S., Grasso S., Grasso R., Grimmer L., Grissom C., Gu Q., Guan X. -D., Guarracino F., Guasch N., Guatteri L., Gueret R., Guerin C., Guerot E., Guitard P. -G., Gul F., Gumus A., Gurjar M., Gutierrez P., Hachimi A., Hadzibegovic A., Hagan S., Hammel C., Han Song J., Hanlon G., Heines S., Henriksson J., Herbrecht J. -E., Heredia Orbegoso G. O., Hermon A., Hernandez R., Hernandez C., Herrera L., Herrera-Gutierrez M., Hidalgo J., Hill D., Holmquist D., Homez M., Hongtao X., Hormis A., Horner D., Hornos M. C., Hou M., House S., Housni B., Hugill K., Humphreys S., Humbert L., Hunter S., Hwa Young L., Iezzi N., Ilutovich S., Inal V., Innes R., Ioannides P., Iotti G. A., Ippolito M., Irie H., Iriyama H., Itagaki T., Izura J., Izza S., Jabeen R., Jamaati H., Jamadarkhana S., Jamoussi A., Jankowski M., Jaramillo L. A., Jeon K., Jeong Lee S., Jeswani D., Jha S., Jiang L., Jing C., Jochmans S., Johnstad B. A., Jongmin L., Joret A., Junhasavasdikul D., Jurado M. T., Kam E., Kamohara H., Kane C., Kara I., Karakurt S., Karnjanarachata C., Kataoka J., Katayama S., Kaushik S., Kelebek Girgin N., Kerr K., Kerslake I., Khairnar P., Khalid A., Khan A., Khanna A. K., Khorasanee R., Kienhorst D., Kirakli C., Knafelj R., Kol M. K., Kongpolprom N., Kopitko C., Korkmaz Ekren P., Kubisz-Pudelko A., Kulcsar Z., Kumasawa J., Kuriyama A., Kutchak F., Labarca E., Labat F., Laborda C., Laca Barrera M. A., Lagache L., Landaverde Lopez A., Lanspa M., Lascari V., Le Meur M., Lee S. H., Lee Y. J., Lee J., Lee W. -Y., Legernaes T., Leiner T., Lemiale V., Leonor T., Lepper P. M., Li D., Li H., Li O., Lima A. R., Lind D., Litton E., Liu N., Liu L., Liu J., Llitjos J. -F., Llorente B., Lopez R., Lopez C. 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C., Wei B. -L., Weller D., Welsh D., Welters I., Wert M., Whiteley S., Wilby E., Williams E., Williams K., Wilson A., Wojtas J., Won Huh J., Wrathall D., Wright C., Wu J. -F., Xi G., Xing Z. -J., Xu H., Yamamoto K., Yan J., Yanez J., Yang X., Yates E., Yazicioglu Mocin O., Ye Z., Yildirim F., Yoshida N., Yoshido H. H. L., Young Lee B., Yu R., Yu G., Yu T., Yuan B., Yuangtrakul N., Yumoto T., Yun X., Zakalik G., Zaki A., Zalba-Etayo B., Zambon M., Zang B., Zani G., Zarka J., Zerbi S. M., Zerman A., Zetterquist H., Zhang J., Zhang H., Zhang W., Zhang G., Zhao H., Zheng J., Zhu B., and Zumaran R.
Abstract: Background: Current management practices and outcomes in weaning from invasive mechanical ventilation are poorly understood. We aimed to describe the epidemiology, management, timings, risk for failure, and outcomes of weaning in patients requiring at least 2 days of invasive mechanical ventilation. Methods: WEAN SAFE was an international, multicentre, prospective, observational cohort study done in 481 intensive care units in 50 countries. Eligible participants were older than 16 years, admitted to a participating intensive care unit, and receiving mechanical ventilation for 2 calendar days or longer. We defined weaning initiation as the first attempt to separate a patient from the ventilator, successful weaning as no reintubation or death within 7 days of extubation, and weaning eligibility criteria based on positive end-expiratory pressure, fractional concentration of oxygen in inspired air, and vasopressors. The primary outcome was the proportion of patients successfully weaned at 90 days. Key secondary outcomes included weaning duration, timing of weaning events, factors associated with weaning delay and weaning failure, and hospital outcomes. This study is registered with ClinicalTrials.gov, NCT03255109. Findings: Between Oct 4, 2017, and June 25, 2018, 10 232 patients were screened for eligibility, of whom 5869 were enrolled. 4523 (77·1%) patients underwent at least one separation attempt and 3817 (65·0%) patients were successfully weaned from ventilation at day 90. 237 (4·0%) patients were transferred before any separation attempt, 153 (2·6%) were transferred after at least one separation attempt and not successfully weaned, and 1662 (28·3%) died while invasively ventilated. The median time from fulfilling weaning eligibility criteria to first separation attempt was 1 day (IQR 0–4), and 1013 (22·4%) patients had a delay in initiating first separation of 5 or more days. Of the 4523 (77·1%) patients with separation attempts, 2927 (64·7%) had a short wean (≤1 d
Published: 2023

15. Oxidized Silicon Terminated Diamond p-MOSFETs with Channel Mobility >150 cm2V-1s-1 and |VTH|> 3V Normally-off for Complementary Power Circuits

Author: Kawarada, H., primary, Ota, K., additional, Fu, Y., additional, Narita, A., additional, Zhu, X., additional, Hiraiwa, A., additional, and Fujishima, T., additional
Published: 2023
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16. Comparative study of macroscopic quantum tunneling in Bi_2Sr_2CaCu_2O_y intrinsic Josephson junctions with different device structures

Author: Ota, K., Hamada, K., Takemura, R., Ohmaki, M., Machi, T., Tanabe, K., Suzuki, M., Maeda, A., and Kitano, H.
Subjects: Condensed Matter - Superconductivity
Abstract: We investigated macroscopic quantum tunneling (MQT) of Bi$_2$Sr$_2$CaCu$_2$O$_y$ intrinsic Josephson junctions (IJJs) with two device structures. One is a nanometer-thick small mesa structure with only two or three IJJs and the other is a stack of a few hundreds of IJJs on a narrow bridge structure. Experimental results of switching current distribution for the first switching events from zero-voltage state showed a good agreement with the conventional theory for a single Josephson junction, indicating that a crossover temperature from thermal activation to MQT regime for the former device structure was as high as that for the latter device structure. Together with the observation of multiphoton transitions between quantized energy levels in MQT regime, these results strongly suggest that the observed MQT behavior is intrinsic to a single IJJ in high-$T_c$ cuprates, independent of device structures. The switching current distribution for the second switching events from the first resistive state, which were carefully distinguished from the first switchings, was also compared between two device structures. In spite of the difference in the heat transfer environment, the second switching events for both devices were found to show a similar temperature-independent behavior up to a much higher temperature than the crossover temperature for the first switching. We argue that it cannot be explained in terms of the self-heating owing to dissipative currents after the first switching. As possible candidates, the MQT process for the second switching and the effective increase of electronic temperature due to quasiparticle injection are discussed., Comment: 10pages, 7figures, submitted to Phys. Rev. B
Published: 2008
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17. Numerical simulation of non-uniform bed-load transport using a Lagrangian method and probabilistic Exner equation

Author: Ota, K., primary and Sato, T., additional
Published: 2020
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18. Complex microwave conductivity of Na-DNA powders

Author: Kitano, H., Ota, K., and Maeda, A.
Subjects: Condensed Matter - Soft Condensed Matter
Abstract: We report the complex microwave conductivity, $\sigma=\sigma_1-i\sigma_2$, of Na-DNA powders, which was measured from 80 K to 300 K by using a microwave cavity perturbation technique. We found that the magnitude of $\sigma_1$ near room temperature was much larger than the contribution of the surrounding water molecules, and that the decrease of $\sigma_1$ with decreasing temperature was sufficiently stronger than that of the conduction of counterions. These results clearly suggest that the electrical conduction of Na-DNA is intrinsically semiconductive., Comment: 16 pages, 7 figures
Published: 2006
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19. Subaru Deep Survey V. A Census of Lyman Break Galaxies at z=4 and 5 in the Subaru Deep Fields: Photometric Properties

Author: Ouchi, M., Shimasaku, K., Okamura, S., Furusawa, H., Kashikawa, N., Ota, K., Doi, M., Hamabe, M., Kimura, M., Komiyama, Y., Miyazaki, M., Miyazaki, S., Nakata, F., Sekiguchi, M., Yagi, M., and Yasuda, N.
Subjects: Astrophysics
Abstract: (abridged) We investigate photometric properties of Lyman Break Galaxies (LBGs) at z=3.5-5.2 based on large samples of 2,600 LBGs detected in deep (i'~27) and wide-field (1,200 arcmin^2) images taken in the Subaru Deep Field (SDF) and the Subaru/XMM Deep Field (SXDF). The selection criteria for the LBG samples are examined with 85 spectroscopically identified objects and by Monte Carlo simulations. We find in the luminosity functions of LBGs (i) that the number density of bright galaxies (M_{1700}<-22; corresponding to SFR_{corr}>100 Msolar yr^{-1}) decreases significantly from z=4 to 5 and (ii) that the faint-end slope of the luminosity function may become steeper towards higher redshifts. We estimate dust extinction of z=4 LBGs with M~0.13., Comment: 41 pages, 22 figures, ApJ in press. Paper with high resolution figures is available at http://hikari.astron.s.u-tokyo.ac.jp/~ouchi/work/astroph/SDS_V_VI/SDS_V.pdf (PDF)
Published: 2003
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20. Subaru Deep Survey VI. A Census of Lyman Break Galaxies at z=4 and 5 in the Subaru Deep Fields: Clustering Properties

Author: Ouchi, M., Shimasaku, K., Okamura, S., Furusawa, H., Kashikawa, N., Ota, K., Doi, M., Hamabe, M., Kimura, M., Komiyama, Y., Miyazaki, M., Miyazaki, S., Nakata, F., Sekiguchi, M., Yagi, M., and Yasuda, N.
Subjects: Astrophysics
Abstract: We investigate the clustering properties of 2,600 Lyman Break Galaxies (LBGs) at z=3.5-5.2 in two large blank fields, the Subaru Deep Field and the Subaru/XMM Deep Field (600arcmin^2 each). The angular correlation functions of these LBGs show a clear clustering at both z~4 and 5. The correlation lengths are r_0= 4.1^{+0.2}_{-0.2} and 5.9^{+1.3}_{-1.7} h_{100}^{-1} Mpc (r_0= 5.1^{+1.0}_{-1.1} and 5.9^{+1.3}_{-1.7} h_{100}^{-1} Mpc) for all the detected LBGs (for L>L* LBGs) at z~4 and 5, respectively. These correlation lengths correspond to galaxy-dark matter biases of b_g= 2.9^{+0.1}_{-0.1} and 4.6^{+0.9}_{-1.2} (b_g=3.5^{+0.6}_{-0.7} and 4.6^{+0.9}_{-1.2}), for all the detected LBGs (for L>L^* LBGs) at z~4 and 5, respectively. These results, combined with estimates for z~3 LBGs in the literature, show that the correlation length of L>L^* LBGs is almost constant, ~5 h_{100}^{-1} Mpc, over z~3-5, while the bias monotonically increases with redshift at z>3. We also find that for LBGs at z~4 the clustering amplitude increases with UV-continuum luminosity and with the amount of dust extinction. We estimate the mass of dark halos hosting various kinds of high-z galaxies including LBGs with the analytic model given by Sheth & Tormen (1999). We find that the typical mass of dark halos hosting L>L^* LBGs is about 1x10^{12} h_{70}^{-1}Msol over z~3-5, which is comparable to that of the Milky Way Galaxy. A single dark halo with ~10^{12} h_{70}^{-1} Msol is found to host 0.1-0.3 LBG on average but host about four K-band selected galaxies., Comment: 33 pages, 12 figures, ApJ in press. Paper with high resolution figures is available at http://hikari.astron.s.u-tokyo.ac.jp/~ouchi/work/astroph/SDS_V_VI/SDS_VI.pdf (PDF) (The abstract was reduced by the revision.)
Published: 2003
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21. Optical Spectropolarimetry of SN 2002ap: High Velocity Asymmetric Explosion

Author: Kawabata, K. S., Jeffery, D. J., Iye, M., Ohyama, Y., Kosugi, G., Kashikawa, N., Ebizuka, N., Sasaki, T., Sekiguchi, K., Nomoto, K., Mazzali, P., Deng, J., Maeda, K., Aoki, K., Saito, Y., Takata, T., Yoshida, M., Asai, R., Inata, M., Okita, K., Ota, K., Ozawa, T., Shimizu, Y., Taguchi, H., Yadoumaru, Y., Misawa, T., Nakata, F., Yamada, T., Tanaka, I., and Kodama, T.
Subjects: Astrophysics
Abstract: We present spectropolarimetry of the Type Ic supernova SN 2002ap and give a preliminary analysis: the data were taken at two epochs, close to and one month later than the visual maximum (2002 February 8). In addition we present June 9 spectropolarimetry without analysis. The data show the development of linear polarization. Distinct polarization profiles were seen only in the O I \lambda 7773 multiplet/Ca II IR triplet absorption trough at maximum light and in the Ca II IR triplet absorption trough a month later, with the latter showing a peak polarization as high as ~2 %. The intrinsic polarization shows three clear position angles: 80 degs for the February continuum, 120 degs for the February line feature, and 150 degs for the March data. We conclude that there are multiple asymmetric components in the ejecta. We suggest that the supernova has a bulk asymmetry with an axial ratio projected on the sky that is different from 1 by of order 10 %. Furthermore, we suggest very speculatively that a high velocity ejecta component moving faster than ~0.115c (e.g., a jet) contributes to polarization in the February epoch., Comment: 7 pages, 3 figures, accepted for publication in the Astrophysical Journal (Letters)
Published: 2002
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22. A Lyα emitter with an extremely large rest-frame equivalent width of ∼900 Å at z = 6.5: A candidate population III-dominated galaxy?

Author: Kashikawa, N, Nagao, T, Toshikawa, J, Ishizaki, Y, Egami, E, Hayashi, M, Ly, C, Malkan, MA, Matsuda, Y, Shimasaku, K, Iye, M, Ota, K, Shibuya, T, Jiang, L, Taniguchi, Y, and Shioya, Y
Subjects: cosmology: observations, early universe, galaxies: formation, galaxies: high-redshift, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We have identified a very interesting Lyα emitter (LAE), whose Lyα emission line has an extremely large observed equivalent width of EW0 = 436+422 - 149 Å, which corresponds to an extraordinarily large intrinsic rest-frame equivalent width of EWint 0 = 872 +844 - 298 Å after the average intergalactic absorption correction. The object was spectroscopically confirmed to be a real LAE by its apparent asymmetric Lyα line profile detected at z = 6.538. The continuum emission of the object was definitely detected in our deep z′-band image; thus, its EW0 was reliably determined. Follow-up deep near-infrared spectroscopy revealed emission lines of neither He II λ1640 as an apparent signature of Population III (Pop III) nor C IV λ1549 as proof of an active nucleus. No detection of the short-lived He II λ1640 line is not necessarily inconsistent with the interpretation that the underlying stellar population of the object is dominated by Pop III. We found that the observed extremely large EW0 of the Lyα emission and the upper limit on the EW0 of the He II λ1640 emission can be explained by population synthesis models favoring a very young age less than 2-4 Myr and massive metal-poor (Z < 10 -5) or even metal-free stars. The observed large EW0 of Lyα is insufficiently explained by Population I/II synthesis models with Z ≥ 10 -3. However, we cannot conclusively rule out the possibility that this object is composed of a normal stellar population with a clumpy dust distribution, which could enhance the Lyα EW0, though its significance is still unclear. © 2012. The American Astronomical Society. All rights reserved..
Published: 2012

23. The stellar population and star formation rates of z ≈ 1.5-1.6[OII]-emitting galaxies selected from narrowband emission-line surveys

Author: Ly, C, Malkan, MA, Kashikawa, N, Hayashi, M, Nagao, T, Shimasaku, K, Ota, K, and Ross, NR
Subjects: galaxies: distances and redshifts, galaxies: evolution, galaxies: high-redshift, galaxies: photometry, galaxies: star formation, infrared: galaxies, ultraviolet: galaxies, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We present the first detailed study of the stellar populations of star-forming galaxies at z ∼ 1.5, which are selected by their [O II] emission line, detected in narrowband surveys. We identified ∼1300 [O II] emitters at z = 1.47 and z = 1.62 in the Subaru Deep Field with rest-frame equivalent widths (EWs) above 13 Å. Optical and near-infrared spectroscopic observations for ≈10% of our samples show that our separation of [O II] from [O III] emission-line galaxies in two-color space is 99% successful. We analyze the multi-wavelength properties of a subset of ∼1200 galaxies with the best photometry. They have average rest-frame EW of 45 Å, stellar mass of 3 × 109 M⊙, and stellar age of 100Myr. In addition, our spectral energy distribution (SED) fitting and broadband colors indicate that [O II] emitters span the full range of galaxy populations at z ∼ 1.5. We also find that 80% of [O II] emitters are also photometrically classified as "BX/BM" (UV) galaxies and/or the star-forming "BzK" (near-IR) galaxies. Our [O II] emission line survey produces a far more complete and somewhat deeper sample of z ∼ 1.5 galaxies than either the BX/BM or sBzK selection alone. We constructed average SEDs and find that higher [O II] EW galaxies have somewhat bluer continua. SED model-fitting shows that they have on average half the stellar mass of galaxies with lower [O II] EW. The observed [O II] luminosity is well correlated with the far-UV continuum with a logarithmic slope of 0.89 ± 0.22. The scatter of the [O II] luminosity against the far-UV continuum suggests that [O II] can be used as a star formation rate indicator with a reliability of 0.23 dex. © 2012. The American Astronomical Society. All rights reserved.
Published: 2012

24. Discovery of a protocluster at z ∼ 6

Author: Toshikawa, J, Kashikawa, N, Ota, K, Morokuma, T, Shibuya, T, Hayashi, M, Nagao, T, Jiang, L, Malkan, MA, Egami, E, Shimasaku, K, Motohara, K, and Ishizaki, Y
Subjects: astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We report the discovery of a protocluster at z∼6 containing at least eight cluster member galaxies with spectroscopic confirmations in the wide-field image of the Subaru Deep Field (SDF). The overdensity of the protocluster is significant at the 6σ level, based on the surface number density of i′-dropout galaxies. The overdense region covers 6′ × 6′ (14 Mpc × 14 Mpc in comoving units at z = 6) and includes 30 i′-dropout galaxies. Follow-up spectroscopy revealed that 15 of these are real z 6 galaxies (5.7 < z < 6.3). Of these 15, 8 are clustering in a narrow redshift range (Δz < 0.05 centered at z = 6.01), corresponding to a seven-fold increase in number density over the average in redshift space. We found no significant difference in the observed properties, such as Lyα luminosities and UV continuum magnitudes, between the eight protocluster members and the seven non-members. The velocity dispersion of the eight protocluster members is 647 ± 124 km s-1, which is about three times higher than that predicted by the standard cold dark matter model. This discrepancy could be attributed to the distinguishing three-dimensional distribution of the eight protocluster members. We discuss two possible explanations for this discrepancy: either the protocluster is already mature, with old galaxies at the center, or it is still immature and composed of three subgroups merging to become a larger cluster. In either case, this concentration of z = 6.01 galaxies in the SDF may be one of the first sites of formation of a galaxy cluster in the universe. © © 2012. The American Astronomical Society. All rights reserved.
Published: 2012

25. Dust attenuation and hαstar formation rates of z ∼ 0.5 galaxies

Author: Ly, C, Malkan, MA, Kashikawa, N, Ota, K, Shimasaku, K, Iye, M, and Currie, T
Subjects: dust, extinction, galaxies: distances and redshifts, galaxies: evolution, galaxies: high-redshift, galaxies: photometry, astro-ph.CO, dust, extinction, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: Using deep narrowband and broadband imaging, we identify 401 z ≈ 0.40 and 249 z ≈ 0.49 Hαline-emitting galaxies in the Subaru Deep Field. Compared to other Hαsurveys at similar redshifts, our samples are unique since they probe lower Hαluminosities, are augmented with multi-wavelength (rest-frame 1000 -1.5 μm) coverage, and a large fraction (20%) of our samples has already been spectroscopically confirmed. Our spectra allow us to measure the Balmer decrement for nearly 60 galaxies with Hβ detected above 5σ. The Balmer decrements indicate an average extinction of A(Hα) = 0.7+1.4-0.7mag. We find that the Balmer decrement systematically increases with higher Hαluminosities and with larger stellar masses, in agreement with previous studies with sparser samples. We find that the star formation rates (SFRs) estimated from modeling the spectral energy distribution (SED) are reliable - we derived an "intrinsic" Hαluminosity which is then reddened assuming the color excess from SED modeling. The SED-predicted Hαluminosity agrees with Hαnarrowband measurements over 3dex (rms of 0.25dex). We then use the SED SFRs to test different statistically based dust corrections for Hαand find that adopting 1mag of extinction is inappropriate: galaxies with lower luminosities are less reddened. We find that the luminosity-dependent dust correction of Hopkins et al. yields consistent results over 3dex (rms of 0.3dex). Our comparisons are only possible by assuming that stellar reddening is roughly half of nebular reddening. The strong correspondence argues that with SED modeling, we can derive reliable intrinsic SFRs even in the absence of Hαmeasurements at z ∼ 0.5. © 2012. The American Astronomical Society. All rights reserved.
Published: 2012

26. Completing the census of Lyα emitters at the reionization Epoch

Author: Kashikawa, N, Shimasaku, K, Matsuda, Y, Egami, E, Jiang, L, Nagao, T, Ouchi, M, Malkan, MA, Hattori, T, Ota, K, Taniguchi, Y, Okamura, S, Ly, C, Iye, M, Furusawa, H, Shioya, Y, Shibuya, T, Ishizaki, Y, and Toshikawa, J
Subjects: cosmology: observations, early universe, galaxies: formation, galaxies: high-redshift, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We carried out extended spectroscopic confirmations of Lyα emitters (LAEs) at z = 6.5 and 5.7 in the Subaru Deep Field. Now, the total number of spectroscopically confirmed LAEs is 45 and 54 at z = 6.5 and 5.7, respectively, and at least 81% (70%) of our photometric candidates at z = 6.5 (5.7) have been spectroscopically identified as real LAEs. We made careful measurements of the Lyα luminosity, both photometrically and spectroscopically, to accurately determine the Lyα and rest-UV luminosity functions (LFs). The substantially improved evaluation of the Lyα LF at z = 6.5 shows an apparent deficit from z = 5.7 at least at the bright end, and a possible decline even at the faint end, though small uncertainties remain. The rest-UV LFs at z = 6.5 and 5.7 are in good agreement, at least at the bright end, in clear contrast to the differences seen in the Lyα LF. These results imply an increase in the neutral fraction of the intergalactic medium from z = 5.7 to 6.5. The rest-frame equivalent width (EW0) distribution at z = 6.5 seems to be systematically smaller than z = 5.7, and it shows an extended tail toward larger EW0. The bright end of the rest-UV LF can be reproduced from the observed Lyα LF and a reasonable EW0-UV luminosity relation. Integrating this rest-UV LF provides the first measurement of the contribution of LAEs to the photon budget required for reionization. The derived UV LF suggests that the fractional contribution of LAEs to the photon budget among Lyman break galaxies significantly increases toward faint magnitudes. Low-luminosity LAEs could dominate the ionizing photon budget, though this inference depends strongly on the uncertain faint-end slope of the Lyα LF. © 2011. The American Astronomical Society. All rights reserved.
Published: 2011

27. Spitzer space telescope constraint on the stellar mass of a z = 6.96 Ly α emitter

Author: Ota, K, Ly, C, Malkan, MA, Motohara, K, Hayashi, M, Shimasaku, K, Morokuma, T, Iye, M, Kashikawa, N, and Hattori, T
Subjects: cosmology: early universe, cosmology: observations, galaxies: high-redshift, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We obtained mid-infrared 3.6 and 4.5μm imaging of a z = 6.96 Lyα emitter (LAE), IOK-1, discovered in the Subaru Deep Field, using Spitzer Space Telescope Infrared Array Camera observations. After removal of a nearby bright source, we found that IOK-1 is not significantly detected in any of these infrared bands to m3:6μm ∼ 24.00 and m4:5μm ∼ 23.54 at 3φ. Fitting population synthesis models to the spectral energy distribution consisting of the upper limit fluxes of the optical-to-infrared non-detection images and fluxes in detection images, we constrained the stellar mass, M*, of IOK-1. This LAE could have either a mass as low as M* . ≤2-9 × 108 M for young age (≤10 Myr) and low dust reddening (AV ∼ 0) or a mass as large as M* . 1-4 × 1010 M for either old age (>100 Myr) or high dust reddening (AV ∼ 1.5). This would be within the range of masses of z ∼ 3-6.6 LAEs studied to date, ∼106-10 10M. Hence, IOK-1 is not a particularly unique galaxy with extremely high mass or low mass, but is similar to one of the LAEs seen at later epochs. © 2010. Astronomical Society of Japan.
Published: 2010

28. Contributors

Author: Aricò, Antonino S., primary, Azzato, Giulia, additional, Backhouse, Rachel, additional, Barba, Daniela, additional, Basile, Angelo, additional, Bellini, Stefano, additional, Blasi, Alessandro, additional, Bossel, Ulf, additional, Bouzek, Karel, additional, Caputo, Giampaolo, additional, Caravella, Alessio, additional, Colozzi, M., additional, Divins, Núria J., additional, Fiorenza, Giuseppe, additional, Fontanille, Pierre, additional, Gallucci, Fausto, additional, Giaconia, Alberto, additional, Giannini, Antonella, additional, Grahl-Madsen, Laila, additional, Green, Ben, additional, Greenhalgh, Daniel A., additional, Hacker, Viktor, additional, Hemmes, K., additional, Hnát, Jaromír, additional, Iaquaniello, G., additional, Iaquaniello, Gaetano, additional, Ishihara, A., additional, Iulianelli, Adolfo, additional, Lammer, Michael, additional, Llorca, Jordi, additional, Martino, Marco, additional, McPhail, Stephen J., additional, Meloni, Eugenio, additional, Meshksar, Maryam, additional, Monteleone, Giulia, additional, Morico, Barbara, additional, Mosca, L., additional, Oldani, Claudio, additional, Ota, K., additional, Pagliaro, Mario, additional, Paidar, Martin, additional, Palma, Vincenzo, additional, Palo, Emma, additional, Rahimpour, Mohammad Reza, additional, Roostaie, Tayebe, additional, Ruocco, Concetta, additional, Salladini, Annarita, additional, Serrano, Isabel, additional, Siracusano, Stefania, additional, Soler, Lluís, additional, Sun, Yu, additional, Taraschi, S., additional, Teplyakov, V., additional, Tonella, Stefano, additional, Turchetti, Luca, additional, Vendrell, Xavier, additional, and Verardi, Alessandra, additional
Published: 2020
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29. Role of green hydrogen for our sustainable growth

Author: Ishihara, A., primary and Ota, K., additional
Published: 2020
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30. Clinical Courses of Graft Failure Caused by Chronic Allograft Dysfunction in Kidney Transplantation

Author: Fujiwara, T., Teruta, S., Tsudaka, S., Ota, K., and Matsuda, H.
Published: 2017
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31. Improvement of curved hole EDM drilling performance using suspended ball electrode by workpiece vibration

Author: Okada, A., Yamaguchi, A., and Ota, K.
Published: 2017
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32. Fabrication process of flexibly patterned grating by interference lithography system with automated beam alignment module

Author: Liddle, J. Alexander, Ruiz, Ricardo, Toyoda, K., Nawaki, Y., Yanoshita, R., Orihara, S., Wasamoto, M., Ota, K., and Tsuruoka, K.
Published: 2024
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33. Impact of Antimicrobial Use at the Start of Mechanical Ventilation on Ventilator-associated Lower Respiratory Tract Infections in Patients With Acute Respiratory Distress Syndrome Related to Coronavirus Disease 2019

Author: Ishii, J., primary, Nishikimi, M., additional, Shimatani, T., additional, Ota, K., additional, Ohshimo, S., additional, and Shime, N., additional
Published: 2023
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34. Kinetic study of oxygen reduction reaction on tantalum oxide-based electrocatalysts produced from oxy-tantalum phthalocyanines in acidic media

Author: Uehara, N., Ishihara, A., Nagai, T., Matsumoto, M., Imai, H., Kohno, Y., Matsuzawa, K., Mitsushima, S., and Ota, K.
Published: 2015
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35. Tantalum oxide-based electrocatalysts made from oxy-tantalum phthalocyanines as non-platinum cathodes for polymer electrolyte fuel cells

Author: Uehara, N., Ishihara, A., Matsumoto, M., Imai, H., Kohno, Y., Matsuzawa, K., Mitsushima, S., and Ota, K.
Published: 2015
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36. Variability-Controlled HfZrO2 Ferroelectric Tunnel Junctions for Reservoir Computing

Author: Ota, K., primary, Yamaguchi, M., additional, Kabuyanagi, S., additional, Fujii, S., additional, Saitoh, M., additional, and Yoshikawa, M., additional
Published: 2022
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37. 58: SARS-COV-2 ANTIBODY CHARACTERISTICS OF SALIVA FROM VACCINATED INDIVIDUALS

Author: Ota, K., primary, Mitsumoto-Kaseida, F., additional, Sakamoto, K., additional, Kosai, K., additional, Hasegawa, H., additional, Yamamoto, K., additional, Izumikawa, K., additional, Mukae, H., additional, Kohno, S., additional, and Yanagihara, K., additional
Published: 2022
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38. Association of PD-L1 overexpression with activating EGFR mutations in surgically resected nonsmall-cell lung cancer

Author: Azuma, K., Ota, K., Kawahara, A., Hattori, S., Iwama, E., Harada, T., Matsumoto, K., Takayama, K., Takamori, S., Kage, M., Hoshino, T., Nakanishi, Y., and Okamoto, I.
Published: 2014
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39. Influence of microstructural characteristics on mechanical properties of ADC12 aluminum alloy

Author: Okayasu, M., Ota, K., Takeuchi, S., Ohfuji, H., and Shiraishi, T.
Published: 2014
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40. Experimental study of back gate bias effect and short channel effect in ultra-thin buried oxide tri-gate nanowire MOSFETs

Author: Ota, K., Saitoh, M., Tanaka, C., and Numata, T.
Published: 2014
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41. Carrier suppression for an optical tunable two-tone generator ranging up to 40 GHz with a compact and high speed phase modulator

Author: Australian Conference on Optical Fibre Technology (39th : 2014 : Melbourne), Oikawa, Y, Toyoda, K, Ota, K, Iwai, H, Inagaki, K, Kawanishi, T, and Shiga, N
Published: 2014

42. EP08.01-036 Low-dose EGFR-TKIs Directly Induce Maturation and Functional Activity of Human Dendritic Cells in an EGFR-independent manner

Author: Inoue, H., primary, Tsutsumi, H., additional, Okamura, K., additional, Ota, K., additional, Yoneshima, Y., additional, Iwama, E., additional, Tanaka, K., additional, and Okamoto, I., additional
Published: 2022
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43. Extraction of Nd3+-doped LiYF4 phosphor from sol–gel-derived oxyfluoride glass ceramics by hydrofluoric acid treatment

Author: Kawamura, G., Yoshimura, R., Ota, K., Oh, S.Y., Muto, H., Hayakawa, T., and Matsuda, A.
Published: 2013
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44. EP.14B.01 Prognostic Impact of Tumour Size in Resected Thymic Epithelial Tumours - A Validation Analysis of the 9th TNM Staging System -

Author: Abe, M., Karashima, T., Abe, Y., Ota, K., Sato, T., Noda, D., Takamori, S., Takumi, Y., Osoegawa, A., and Sugio, K.
Published: 2024
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45. The effect of bolus volume on laryngeal closure and UES opening in swallowing: Kinematic analysis using 320‐row area detector CT study

Author: Shibata, S., Inamoto, Y., Saitoh, E., Kagaya, H., Aoyagi, Y., Ota, K., Akahori, R., Fujii, N., Palmer, J. B., and González-Fernández, M.
Published: 2017
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46. Prolonged matrix metalloproteinase-3 high expression after cyclic compressive load on human synovial cells in three-dimensional cultured tissue

Author: Akamine, Y., Kakudo, K., Kondo, M., Ota, K., Muroi, Y., Yoshikawa, H., and Nakata, K.
Published: 2012
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47. Investigation on sandy riverbank failure eroded by water level rising

Author: Arai, R., primary, Ota, K., additional, Sato, T., additional, and Toyoda, Y., additional
Published: 2016
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48. High-resolution dating of surface peat based on 137Cs and 210Pb radioactivity concentration.

Author: Tsuneoka, R., Yokoyama, T., Ota, K., Miyairi, Y., Kondo, K., Yokochi, M., Kaneko, K., Inoue, T., Kito, N., Uemura, K., Sumita, Mari, Momohara, A., Fujita, H., Tsuneoka, R., Yokoyama, T., Ota, K., Miyairi, Y., Kondo, K., Yokochi, M., Kaneko, K., Inoue, T., Kito, N., Uemura, K., Sumita, Mari, Momohara, A., and Fujita, H.
Published: 2022

49. Effects of junction geometry in crossover temperature to macroscopic quantum tunneling regime of intrinsic Josephson junctions

Author: Kitano, H., Ishikawa, K., Takekoshi, S., Ota, K., and Maeda, A.
Published: 2011
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50. The Japanese Interferon Study Group (JISG) has established the efficacy of human interferon-β for serious CMV pneumonitis in kidney recipients

Author: the JISG, Takahashi, K., Teraoka, S., Ota, K., Kosaki, M., Okazaki, H., Kootstra, Gauke, editor, Opelz, Gerhard, editor, Buurman, W. A., editor, van Hooff, J. P., editor, MacMaster, P., editor, and Wallwork, J., editor
Published: 1992
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