Search

Your search keyword '"Oshima, T."' showing total 3,523 results
Start Over Author "Oshima, T." Publication Year Range Last 50 years
3,523 results on '"Oshima, T."'

2. Large format imaging spectrograph for the Large Submillimeter Telescope (LST)

Author

Kohno, K., Kawabe, R., Tamura, Y., Endo, A., Baselmans, J. J. A., Karatsu, K., Inoue, A. K., Moriwaki, K., Hayatsu, N. H., Yoshida, N., Yoshimura, Y., Hatsukade, B., Umehata, H., Oshima, T., Takekoshi, T., Taniguchi, A., Klaassen, P. D., Mroczkowski, T., Cicone, C., Bertoldi, F., Dannerbauer, H., and Tosaki, T.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present a conceptual study of a large format imaging spectrograph for the Large Submillimeter Telescope (LST) and the Atacama Large Aperture Submillimeter Telescope (AtLAST). Recent observations of high-redshift galaxies indicate the onset of earliest star formation just a few 100 million years after the Big Bang (i.e., z = 12--15), and LST/AtLAST will provide a unique pathway to uncover spectroscopically-identified first forming galaxies in the pre-reionization era, once it will be equipped with a large format imaging spectrograph. We propose a 3-band (200, 255, and 350 GHz), medium resolution (R = 2,000) imaging spectrograph with 1.5 M detectors in total based on the KATANA concept (Karatsu et al. 2019), which exploits technologies of the integrated superconducting spectrometer (ISS) and a large-format imaging array. A 1-deg2 drilling survey (3,500 hr) will capture a large number of [O III] 88 um (and [C II] 158 um) emitters at z = 8--9, and constrain [O III] luminosity functions at z > 12., Comment: Presented at SPIE Astronomical Telescopes + Instrumentation 2020. Full published paper and video available at http://dx.doi.org/10.1117/12.2561238 See also https://www.lstobservatory.org for the LST project

Published
2021
Full Text
View/download PDF

3. Proton penetration efficiency over a high altitude observatory in Mexico

Author

S. Miyake, T. Koi, Y. Muraki, Y. Matsubara, S. Masuda, P. Miranda, T. Naito, E. Ortiz, A. Oshima, T. Sakai, T. Sako, S. Shibata, H. Takamaru, M. Tokumaru, J. F. Valdés-Galicia

Subjects
Physics, QC1-999
Abstract

In association with a large solar flare on November 7, 2004, the solar neutron detectors located at Mt. Chacaltaya (5,250 m) in Bolivia and Mt. Sierra Negra (4,600 m) in Mexico recorded very interesting events. In order to explain these events, we have performed a calculation solving the equation of motion of anti-protons inside the magnetosphere. Based on these results, the Mt. Chacaltaya event may be explained by the detection of solar neutrons, while the Mt. Sierra Negra event may be explained by the first detection of very high energy solar neutron decay protons (SNDPs) around 6 GeV.

Published
2023
Full Text
View/download PDF

4. Extremely-bright submillimeter galaxies beyond the Lupus-I star-forming region

Author

Tamura, Y., Kawabe, R., Shimajiri, Y., Tsukagoshi, T., Nakajima, Y., Oasa, Y., Wilner, D. J., Chandler, C. J., Saigo, K., Tomida, K., Yun, M. S., Taniguchi, A., Kohno, K., Hatsukade, B., Aretxaga, I., Austermann, J. E., Dickman, R., Ezawa, H., Goss, W. M., Hayashi, M., Hughes, D. H., Hiramatsu, M., Inutsuka, S., Ogasawara, R., Ohashi, N., Oshima, T., Scott, K. S., and Wilson, G. W.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We report detections of two candidate distant submillimeter galaxies (SMGs), MM J154506.4$-$344318 and MM J154132.7$-$350320, which are discovered in the AzTEC/ASTE 1.1 mm survey toward the Lupus-I star-forming region. The two objects have 1.1 mm flux densities of 43.9 and 27.1 mJy, and have Herschel/SPIRE counterparts as well. The Submillimeter Array counterpart to the former SMG is identified at 890 $\mu$m and 1.3 mm. Photometric redshift estimates using all available data from the mid-infrared to the radio suggest that the redshifts of the two SMGs are $z_{\rm photo} \simeq$ 4-5 and 3, respectively. Near-infrared objects are found very close to the SMGs and they are consistent with low-$z$ ellipticals, suggesting that the high apparent luminosities can be attributed to gravitational magnification. The cumulative number counts at $S_{\rm 1.1mm} \ge 25$ mJy, combined with other two 1.1-mm brightest sources, are $0.70 ^{+0.56}_{-0.34}$ deg$^{-2}$, which is consistent with a model prediction that accounts for flux magnification due to strong gravitational lensing. Unexpectedly, a $z > 3$ SMG and a Galactic dense starless core (e.g., a first hydrostatic core) could be similar in the mid-infrared to millimeter spectral energy distributions and spatial structures at least at $\gtrsim 1"$. This indicates that it is necessary to distinguish the two possibilities by means of broad band photometry from the optical to centimeter and spectroscopy to determine the redshift, when a compact object is identified toward Galactic star-forming regions., Comment: Accepted for publication in ApJ. 16 pages, 9 figures, 2 tables

Published
2015
Full Text
View/download PDF

7. The Physics of the B Factories

Author

Bevan, A. J., Golob, B., Mannel, Th., Prell, S., Yabsley, B. D., Abe, K., Aihara, H., Anulli, F., Arnaud, N., Aushev, T., Beneke, M., Beringer, J., Bianchi, F., Bigi, I. I., Bona, M., Brambilla, N., rodzicka, J. B, Chang, P., Charles, M. J., Cheng, C. H., Cheng, H. -Y., Chistov, R., Colangelo, P., Coleman, J. P., Drutskoy, A., Druzhinin, V. P., Eidelman, S., Eigen, G., Eisner, A. M., Faccini, R., Flood, K. T ., Gambino, P., Gaz, A., Gradl, W., Hayashii, H., Higuchi, T., Hulsbergen, W. D., Hurth, T., Iijima, T., Itoh, R., Jackson, P. D., Kass, R., Kolomensky, Yu. G., Kou, E., Križan, P., Kronfeld, A., Kumano, S., Kwon, Y. J., Latham, T. E., Leith, D. W. G. S., Lüth, V., Martinez-Vidal, F., Meadows, B. T., Mussa, R., Nakao, M., Nishida, S., Ocariz, J., Olsen, S. L., Pakhlov, P., Pakhlova, G., Palano, A., Pich, A., Playfer, S., Poluektov, A., Porter, F. C., Robertson, S. H., Roney, J. M., Roodman, A., Sakai, Y., Schwanda, C., Schwartz, A. J., Seidl, R., Sekula, S. J., Steinhauser, M., Sumisawa, K., Swanson, E. S., Tackmann, F., Trabelsi, K., Uehara, S., Uno, S., van der Water, R., Vasseur, G., Verkerke, W., Waldi, R., Wang, M. Z., Wilson, F. F., Zupan, J., Zupanc, A., Adachi, I., Albert, J., Banerjee, Sw., Bellis, M., Ben-Haim, E., Biassoni, P., Cahn, R. N., Cartaro, C., Chauveau, J., Chen, C., Chiang, C. C., Cowan, R., Dalseno, J., Davier, M., Davies, C., Dingfelder, J. C., nard, B. Eche, Epifanov, D., Fulsom, B. G., Gabareen, A. M., Gary, J. W., Godang, R., Graham, M. T., Hafner, A., Hamilton, B., Hartmann, T., Hayasaka, K., Hearty, C., Iwasaki, Y., Khodjamirian, A., Kusaka, A., Kuzmin, A., Lafferty, G. D., Lazzaro, A., Li, J., Lindemann, D., Long, O., Lusiani, A., Marchiori, G., Martinelli, M., Miyabayashi, K., Mizuk, R., Mohanty, G. B., Muller, D. R., Nakazawa, H., Ongmongkolkul, P., Pacetti, S., Palombo, F., Pedlar, T. K., Piilonen, L. E., Pilloni, A., Poireau, V., Prothmann, K., Pulliam, T., Rama, M., Ratcliff, B. N., Roudeau, P., Schrenk, S., Schroeder, T., Schubert, K. R., Shen, C. P., Shwartz, B., Soffer, A., Solodov, E. P., Somov, A., Starič, M., Stracka, S., Telnov, A. V., Todyshev, K. Yu., Tsuboyama, T., Uglov, T., Vinokurova, A., Walsh, J. J., Watanabe, Y., Won, E., Wormser, G., Wright, D. H., Ye, S., Zhang, C. C., Abachi, S., Abashian, A., Abe, N., Abe, R., Abe, T., Abrams, G. S., Adam, I., Adamczyk, K., Adametz, A., Adye, T., Agarwal, A., Ahmed, H., Ahmed, M., Ahmed, S., Ahn, B. S., Ahn, H. S., Aitchison, I. J. R., Akai, K., Akar, S., Akatsu, M., Akemoto, M., Akhmetshin, R., Akre, R., Alam, M. S., Albert, J. N., Aleksan, R., Alexander, J. P., Alimonti, G., Allen, M. T., Allison, J., Allmendinger, T., Alsmiller, J. R. G., Altenburg, D., Alwyn, K. E., An, Q., Anderson, J., Andreassen, R., Andreotti, D., Andreotti, M., Andress, J. C., Angelini, C., Anipko, D., Anjomshoaa, A., Anthony, P. L., Antillon, E. A., Antonioli, E., Aoki, K., Arguin, J. F., Arinstein, K., Arisaka, K., Asai, K., Asai, M., Asano, Y., Asgeirsson, D. J., Asner, D. M., Aso, T., Aspinwall, M. L., Aston, D., Atmacan, H., Aubert, B., Aulchenko, V., Ayad, R., Azemoon, T., Aziz, T., Azzolini, V., Azzopardi, D. E., Baak, M. A., Back, J. J., Bagnasco, S., Bahinipati, S., Bailey, D. S., Bailey, S., Bailly, P., van Bakel, N., Bakich, A. M., Bala, A., Balagura, V., Baldini-Ferroli, R., Ban, Y., Banas, E., Band, H. R., Banerjee, S., Baracchini, E., Barate, R., Barberio, E., Barbero, M., Bard, D. J., Barillari, T., Barlow, N. R., Barlow, R. J., Barrett, M., Bartel, W., Bartelt, J., Bartoldus, R., Batignani, G., Battaglia, M., Bauer, J. M., Bay, A., Beaulieu, M., Bechtle, P., Beck, T. W., Becker, J., Becla, J., Bedny, I., Behari, S., Behera, P. K., Behn, E., Behr, L., Beigbeder, C., Beiline, D., Bell, R., Bellini, F., Bellodi, G., Belous, K., Benayoun, M., Benelli, G., Benitez, J. F., Benkebil, M., Berger, N., Bernabeu, J., Bernard, D., Bernet, R., Bernlochner, F. U., Berryhill, J. W., Bertsche, K., Besson, P., Best, D. S., Bettarini, S., Bettoni, D., Bhardwaj, V., Bhimji, W., Bhuyan, B., Biagini, M. E., Biasini, M., van Bibber, K., Biesiada, J., Bingham, I., Bionta, R. M., Bischofberger, M., Bitenc, U., Bizjak, I., Blanc, F., Blaylock, G., Blinov, V. E., Bloom, E., Bloom, P. C., Blount, N. L., Blouw, J., Bly, M., Blyth, S., Boeheim, C. T., Bomben, M., Bondar, A., Bondioli, M., Bonneaud, G. R., Bonvicini, G., Booke, M., Booth, J., Borean, C., Borgland, A. W., Borsato, E., Bosi, F., Bosisio, L., Botov, A. A., Bougher, J., Bouldin, K., Bourgeois, P., Boutigny, D., Bowerman, D. A., Boyarski, A. M., Boyce, R. F., Boyd, J. T., Bozek, A., Bozzi, C., Bračko, M., Brandenburg, G., Brandt, T., Brau, B., Brau, J., Breon, A. B., Breton, D., Brew, C., Briand, H., Bright-Thomas, P. G., Brigljević, V., Britton, D. I., Brochard, F., Broomer, B., Brose, J., Browder, T. E., Brown, C. L., Brown, C. M., Brown, D. N., Browne, M., Bruinsma, M., Brunet, S., Bucci, F., Buchanan, C., Buchmueller, O. L., Bünger, C., Bugg, W., Bukin, A. D., Bula, R., Bulten, H., Burchat, P. R., Burgess, W., Burke, J. P., Button-Shafer, J., Buzykaev, A. R., Buzzo, A., Cai, Y., Calabrese, R., Calcaterra, A., Calderini, G., Camanzi, B., Campagna, E., Campagnari, C., Capra, R., Carassiti, V., Carpinelli, M., Carroll, M., Casarosa, G., Casey, B. C. K., Cason, N. M., Castelli, G., Cavallo, N., Cavoto, G., Cecchi, A., Cenci, R., Cerizza, G., Cervelli, A., Ceseracciu, A., Chai, X., Chaisanguanthum, K. S., Chang, M. C., Chang, Y. H., Chang, Y. W., Chao, D. S., Chao, M., Chao, Y., Charles, E., Chavez, C. A., Cheaib, R., Chekelian, V., Chen, A., Chen, E., Chen, G. P., Chen, H. F., Chen, J. -H., Chen, J. C., Chen, K. F., Chen, P., Chen, S., Chen, W. T., Chen, X., Chen, X. R., Chen, Y. Q., Cheng, B., Cheon, B. G., Chevalier, N., Chia, Y. M., Chidzik, S., Chilikin, K., Chistiakova, M. V., Cizeron, R., Cho, I. S., Cho, K., Chobanova, V., Choi, H. H. F., Choi, K. S., Choi, S. K., Choi, Y., Choi, Y. K., Christ, S., Chu, P. H., Chun, S., Chuvikov, A., Cibinetto, G., Cinabro, D., Clark, A. R., Clark, P. J., Clarke, C. K., Claus, R., Claxton, B., Clifton, Z. C., Cochran, J., Cohen-Tanugi, J., Cohn, H., Colberg, T., Cole, S., Colecchia, F., Condurache, C., Contri, R., Convert, P., Convery, M. R., Cooke, P., Copty, N., Cormack, C. M., Corso, F. Dal, Corwin, L. A., Cossutti, F., Cote, D., Ramusino, A. Cotta, Cottingham, W. N., Couderc, F., Coupal, D. P., Covarelli, R., Cowan, G., Craddock, W. W., Crane, G., Crawley, H. B., Cremaldi, L., Crescente, A., Cristinziani, M., Crnkovic, J., Crosetti, G., Cuhadar-Donszelmann, T., Cunha, A., Curry, S., D'Orazio, A., Dû, S., Dahlinger, G., Dahmes, B., Dallapiccola, C., Danielson, N., Danilov, M., Das, A., Dash, M., Dasu, S., Datta, M., Daudo, F., Dauncey, P. D., David, P., Davis, C. L., Day, C. T., De Mori, F., De Domenico, G., De Groot, N., De la Vaissière, C., de la Vaissière, Ch., de Lesquen, A., De Nardo, G., de Sangro, R., De Silva, A., DeBarger, S., Decker, F. J., Sanchez, P. del Amo, Del Buono, L., Del Gamba, V., del Re, D., Della Ricca, G., Denig, A. G., Derkach, D., Derrington, I. M., DeStaebler, H., Destree, J., Devmal, S., Dey, B., Di Girolamo, B., Di Marco, E., Dickopp, M., Dima, M. O., Dittrich, S., Dittongo, S., Dixon, P., Dneprovsky, L., Dohou, F., Doi, Y., Doležal, Z., Doll, D. A., Donald, M., Dong, L., Dong, L. Y., Dorfan, J., Dorigo, A., Dorsten, M. P., Dowd, R., Dowdell, J., Drásal, Z., Dragic, J., Drummond, B. W., Dubitzky, R. S., Dubois-Felsmann, G. P., Dubrovin, M. S., Duh, Y. C., Duh, Y. T., Dujmic, D., Dungel, W., Dunwoodie, W., Dutta, D., Dvoretskii, A., Dyce, N., Ebert, M., Eckhart, E. A., Ecklund, S., Eckmann, R., Eckstein, P., Edgar, C. L., Edwards, A. J., Egede, U., Eichenbaum, A. M., Elmer, P., Emery, S., Enari, Y., Enomoto, R., Erdos, E., Erickson, R., Ernst, J. A., Erwin, R. J., Escalier, M., Eschenburg, V., Eschrich, I., Esen, S., Esteve, L., Evangelisti, F., Everton, C. W., Eyges, V., Fabby, C., Fabozzi, F., Fahey, S., Falbo, M., Fan, S., Fang, F., Fanin, C., Farbin, A., Farhat, H., Fast, J. E., Feindt, M., Fella, A., Feltresi, E., Ferber, T., Fernholz, R. E., Ferrag, S., Ferrarotto, F., Ferroni, F., Field, R. C., Filippi, A., Finocchiaro, G., Fioravanti, E., da Costa, J. Firmino, Fischer, P. -A., Fisher, A., Fisher, P. H., Flacco, C. J., Flack, R. L., Flaecher, H. U., Flanagan, J., Flanigan, J. M., Ford, K. E., Ford, W. T., Forster, I. J., Forti, A. C., Forti, F., Fortin, D., Foster, B., Foulkes, S. D., Fouque, G., Fox, J., Franchini, P., Sevilla, M. Franco, Franek, B., Frank, E. D., Fransham, K. B., Fratina, S., Fratini, K., Frey, A., Frey, R., Friedl, M., Fritsch, M., Fry, J. R., Fujii, H., Fujikawa, M., Fujita, Y., Fujiyama, Y., Fukunaga, C., Fukushima, M., Fullwood, J., Funahashi, Y., Funakoshi, Y., Furano, F., Furman, M., Furukawa, K., Futterschneider, H., Gabathuler, E., Gabriel, T. A., Gabyshev, N., Gaede, F., Gagliardi, N., Gaidot, A., Gaillard, J. -M., Gaillard, J. R., Galagedera, S., Galeazzi, F., Gallo, F., Gamba, D., Gamet, R., Gan, K. K., Gandini, P., Ganguly, S., Ganzhur, S. F., Gao, Y. Y., Gaponenko, I., Garmash, A., Tico, J. Garra, Garzia, I., Gaspero, M., Gastaldi, F., Gatto, C., Gaur, V., Geddes, N. I., Geld, T. L., Genat, J. -F., George, K. A., George, M., George, S., Georgette, Z., Gershon, T. J., Gill, M. S., Gillard, R., Gilman, J. D., Giordano, F., Giorgi, M. A., Giraud, P. -F., Gladney, L., Glanzman, T., Glattauer, R., Go, A., Goetzen, K., Goh, Y. M., Gokhroo, G., Goldenzweig, P., Golubev, V. B., Gopal, G. P., Gordon, A., Gorišek, A., Goriletsky, V. I., Gorodeisky, R., Gosset, L., Gotow, K., Gowdy, S. J., Graffin, P., Grancagnolo, S., Grauges, E., Graziani, G., Green, M. G., Greene, M. G., Grenier, G. J., Grenier, P., Griessinger, K., Grillo, A. A., Grinyov, B. V., Gritsan, A. V., Grosdidier, G., Perdekamp, M. Grosse, Grosso, P., Grothe, M., Groysman, Y., Grünberg, O., Guido, E., Guler, H., Gunawardane, N. J. W., Guo, Q. H., Guo, R. S., Guo, Z. J., Guttman, N., Ha, H., Ha, H. C., Haas, T., Haba, J., Hachtel, J., Hadavand, H. K., Hadig, T., Hagner, C., Haire, M., Haitani, F., Haji, T., Haller, G., Halyo, V., Hamano, K., Hamasaki, H., de Monchenault, G. Hamel, Hamilton, J., Hamilton, R., Hamon, O., Han, B. Y., Han, Y. L., Hanada, H., Hanagaki, K., Handa, F., Hanson, J. E., Hanushevsky, A., Hara, K., Hara, T., Harada, Y., Harrison, P. F., Harrison, T. J., Harrop, B., Hart, A. J., Hart, P. A., Hartfiel, B. L., Harton, J. L., Haruyama, T., Hasan, A., Hasegawa, Y., Hast, C., Hastings, N. C., Hasuko, K., Hauke, A., Hawkes, C. M., Hayashi, K., Hazumi, M., Hee, C., Heenan, E. M., Heffernan, D., Held, T., Henderson, R., Henderson, S. W., Hertzbach, S. S., Hervé, S., Heß, M., Heusch, C. A., Hicheur, A., Higashi, Y., Higasino, Y., Higuchi, I., Hikita, S., Hill, E. J., Himel, T., Hinz, L., Hirai, T., Hirano, H., Hirschauer, J. F., Hitlin, D. G., Hitomi, N., Hodgkinson, M. C., Höcker, A., Hoi, C. T., Hojo, T., Hokuue, T., Hollar, J. J., Hong, T. M., Honscheid, K., Hooberman, B., Hopkins, D. A., Horii, Y., Hoshi, Y., Hoshina, K., Hou, S., Hou, W. S., Hryn'ova, T., Hsiung, Y. B., Hsu, C. L., Hsu, S. C., Hu, H., Hu, T., Huang, H. C., Huang, T. J., Huang, Y. C., Huard, Z., Huffer, M. E., Hufnagel, D., Hung, T., Hutchcroft, D. E., Hyun, H. J., Ichizawa, S., Igaki, T., Igarashi, A., Igarashi, S., Igarashi, Y., Igonkina, O., Ikado, K., Ikeda, H., Ikeda, K., Ilic, J., Inami, K., Innes, W. R., Inoue, Y., Ishikawa, A., Ishino, H., Itagaki, K., Itami, S., Itoh, K., Ivanchenko, V. N., Iverson, R., Iwabuchi, M., Iwai, G., Iwai, M., Iwaida, S., Iwamoto, M., Iwasaki, H., Iwasaki, M., Iwashita, T., Izen, J. M., Jackson, D. J., Jackson, F., Jackson, G., Jackson, P. S., Jacobsen, R. G., Jacoby, C., Jaegle, I., Jain, V., Jalocha, P., Jang, H. K., Jasper, H., Jawahery, A., Jayatilleke, S., Jen, C. M., Jensen, F., Jessop, C. P., Ji, X. B., John, M. J. J., Johnson, D. R., Johnson, J. R., Jolly, S., Jones, M., Joo, K. K., Joshi, N., Joshi, N. J., Judd, D., Julius, T., Kadel, R. W., Kadyk, J. A., Kagan, H., Kagan, R., Kah, D. H., Kaiser, S., Kaji, H., Kajiwara, S., Kakuno, H., Kameshima, T., Kaminski, J., Kamitani, T., Kaneko, J., Kang, J. H., Kang, J. S., Kani, T., Kapusta, P., Karbach, T. M., Karolak, M., Karyotakis, Y., Kasami, K., Katano, G., Kataoka, S. U., Katayama, N., Kato, E., Kato, Y., Kawai, H., Kawai, M., Kawamura, N., Kawasaki, T., Kay, J., Kay, M., Kelly, M. P., Kelsey, M. H., Kent, N., Kerth, L. T., Khan, A., Khan, H. R., Kharakh, D., Kibayashi, A., Kichimi, H., Kiesling, C., Kikuchi, M., Kikutani, E., Kim, B. H., Kim, C. H., Kim, D. W., Kim, H., Kim, H. J., Kim, H. O., Kim, H. W., Kim, J. B., Kim, J. H., Kim, K. T., Kim, M. J., Kim, P., Kim, S. K., Kim, S. M., Kim, T. H., Kim, Y. I., Kim, Y. J., King, G. J., Kinoshita, K., Kirk, A., Kirkby, D., Kitayama, I., Klemetti, M., Klose, V., Klucar, J., Knecht, N. S., Knoepfel, K. J., Knowles, D. J., Ko, B. R., Kobayashi, N., Kobayashi, S., Kobayashi, T., Kobel, M. J., Koblitz, S., Koch, H., Kocian, M. L., Kodyš, P., Koeneke, K., Kofler, R., Koike, S., Koishi, S., Koiso, H., Kolb, J. A., Kolya, S. D., Kondo, Y., Konishi, H., Koppenburg, P., Koptchev, V. B., Kordich, T. M. B., Korol, A. A., Korotushenko, K., Korpar, S., Kouzes, R. T., Kovalskyi, D., Kowalewski, R., Kozakai, Y., Kozanecki, W., Kral, J. F., Krasnykh, A., Krause, R., Kravchenko, E. A., Krebs, J., Kreisel, A., Kreps, M., Krishnamurthy, M., Kroeger, R., Kroeger, W., Krokovny, P., Kronenbitter, B., Kroseberg, J., Kubo, T., Kuhr, T., Kukartsev, G., Kulasiri, R., Kulikov, A., Kumar, R., Kumar, S., Kumita, T., Kuniya, T., Kunze, M., Kuo, C. C., Kuo, T. -L., Kurashiro, H., Kurihara, E., Kurita, N., Kuroki, Y., Kurup, A., Kutter, P. E., Kuznetsova, N., Kvasnička, P., Kyberd, P., Kyeong, S. H., Lacker, H. M., Lae, C. K., Lamanna, E., Lamsa, J., Lanceri, L., Landi, L., Lang, M. I., Lange, D. J., Lange, J. S., Langenegger, U., Langer, M., Lankford, A. J., Lanni, F., Laplace, S., Latour, E., Lau, Y. P., Lavin, D. R., Layter, J., Lebbolo, H., LeClerc, C., Leddig, T., Leder, G., Diberder, F. Le, Lee, C. L., Lee, J., Lee, J. S., Lee, M. C., Lee, M. H., Lee, M. J., Lee, S. -J., Lee, S. E., Lee, S. H., Lee, Y. J., Lees, J. P., Legendre, M., Leitgab, M., Leitner, R., Leonardi, E., Leonidopoulos, C., Lepeltier, V., Leruste, Ph., Lesiak, T., Levi, M. E., Levy, S. L., Lewandowski, B., Lewczuk, M. J., Lewis, P., Li, H., Li, H. B., Li, S., Li, X., Li, Y., Gioi, L. Li, Libby, J., Lidbury, J., Lillard, V., Lim, C. L., Limosani, A., Lin, C. S., Lin, J. Y., Lin, S. W., Lin, Y. S., Lindquist, B., Lindsay, C., Lista, L., Liu, C., Liu, F., Liu, H., Liu, H. M., Liu, J., Liu, R., Liu, T., Liu, Y., Liu, Z. Q., Liventsev, D., Vetere, M. Lo, Locke, C. B., Lockman, W. S., Di Lodovico, F., Lombardo, V., London, G. W., Pegna, D. Lopes, Lopez, L., Lopez-March, N., Lory, J., LoSecco, J. M., Lou, X. C., Louvot, R., Lu, A., Lu, C., Lu, M., Lu, R. S., Lueck, T., Luitz, S., Lukin, P., Lund, P., Luppi, E., Lutz, A. M., Lutz, O., Lynch, G., Lynch, H. L., Lyon, A. J., Lyubinsky, V. R., MacFarlane, D. B., Mackay, C., MacNaughton, J., Macri, M. M., Madani, S., Mader, W. F., Majewski, S. A., Majumder, G., Makida, Y., Malaescu, B., Malaguti, R., Malclès, J., Mallik, U., Maly, E., Mamada, H., Manabe, A., Mancinelli, G., Mandelkern, M., Mandl, F., Manfredi, P. F., Mangeol, D. J. J., Manoni, E., Mao, Z. P., Margoni, M., Marker, C. E., Markey, G., Marks, J., Marlow, D., Marques, V., Marsiske, H., Martellotti, S., Martin, E. C., Martin, J. P., Martin, L., Martinez, A. J., Marzolla, M., Mass, A., Masuzawa, M., Mathieu, A., Matricon, P., Matsubara, T., Matsuda, T., Matsumoto, H., Matsumoto, S., Matsumoto, T., Matsuo, H., Mattison, T. S., Matvienko, D., Matyja, A., Mayer, B., Mazur, M. A., Mazzoni, M. A., McCulloch, M., McDonald, J., McFall, J. D., McGrath, P., McKemey, A. K., McKenna, J. A., Mclachlin, S. E., McMahon, S., McMahon, T. R., McOnie, S., Medvedeva, T., Melen, R., Mellado, B., Menges, W., Menke, S., Merchant, A. M., Merkel, J., Messner, R., Metcalfe, S., Metzler, S., Meyer, N. T., Meyer, T. I., Meyer, W. T., Michael, A. K., Michelon, G., Michizono, S., Micout, P., Miftakov, V., Mihalyi, A., Mikami, Y., Milanes, D. A., Milek, M., Mimashi, T., Minamora, J. S., Mindas, C., Minutoli, S., Mir, L. M., Mishra, K., Mitaroff, W., Miyake, H., Miyashita, T. S., Miyata, H., Miyazaki, Y., Moffitt, L. C., Mohapatra, A., Mohapatra, A. K., Mohapatra, D., Moll, A., Moloney, G. R., Mols, J. P., Mommsen, R. K., Monge, M. R., Monorchio, D., Moore, T. B., Moorhead, G. F., de Freitas, P. Mora, Morandin, M., Morgan, N., Morgan, S. E., Morganti, M., Morganti, S., Mori, S., Mori, T., Morii, M., Morris, J. P., Morsani, F., Morton, G. W., Moss, L. J., Mouly, J. P., Mount, R., Mueller, J., Müller-Pfefferkorn, R., Mugge, M., Muheim, F., Muir, A., Mullin, E., Munerato, M., Murakami, A., Murakami, T., Muramatsu, N., Musico, P., Nagai, I., Nagamine, T., Nagasaka, Y., Nagashima, Y., Nagayama, S., Nagel, M., Naisbit, M. T., Nakadaira, T., Nakahama, Y., Nakajima, M., Nakajima, T., Nakamura, I., Nakamura, T., Nakamura, T. T., Nakano, E., Nakayama, H., Nam, J. W., Narita, S., Narsky, I., Nash, J . A., Natkaniec, Z., Nauenberg, U., Nayak, M., Neal, H., Nedelkovska, E., Negrini, M., Neichi, K., Nelson, D., Nelson, S., Neri, N., Nesom, G., Neubauer, S., Newman-Coburn, D., Ng, C., Nguyen, X., Nicholson, H., Niebuhr, C., Nief, J. Y., Niiyama, M., Nikolich, M. B., Nisar, N. K., Nishimura, K., Nishio, Y., Nitoh, O., Nogowski, R., Noguchi, S., Nomura, T., Nordby, M., Nosochkov, Y., Novokhatski, A., Nozaki, S., Nozaki, T., Nugent, I. M., O'Grady, C. P., O'Neale, S. W., O'Neill, F. G., Oberhof, B., Oddone, P. J., Ofte, I., Ogawa, A., Ogawa, K., Ogawa, S., Ogawa, Y., Ohkubo, R., Ohmi, K., Ohnishi, Y., Ohno, F., Ohshima, T., Ohshima, Y., Ohuchi, N., Oide, K., Oishi, N., Okabe, T., Okazaki, N., Okazaki, T., Okuno, S., Olaiya, E. O., Olivas, A., Olley, P., Olsen, J., Ono, S., Onorato, G., Onuchin, A. P., Onuki, Y., Ooba, T., Orimoto, T. J., Oshima, T., Osipenkov, I. L., Ostrowicz, W., Oswald, C., Otto, S., Oyang, J., Oyanguren, A., Ozaki, H., Ozcan, V. E., Paar, H. P., Padoan, C., Paick, K., Palka, H., Pan, B., Pan, Y., Vazquez, W. Panduro, Panetta, J., Panova, A. I., Panvini, R. S., Panzenböck, E., Paoloni, E., Paolucci, P., Pappagallo, M., Paramesvaran, S., Park, C. S., Park, C. W., Park, H., Park, H. K., Park, K. S., Park, W., Parry, R. J., Parslow, N., Passaggio, S., Pastore, F. C., Patel, P. M., Patrignani, C., Patteri, P., Pavel, T., Pavlovich, J., Payne, D. J., Peak, L. S., Peimer, D. R., Pelizaeus, M., Pellegrini, R., Pelliccioni, M., Peng, C. C., Peng, J. C., Peng, K. C., Peng, T., Penichot, Y., Pennazzi, S., Pennington, M. R., Penny, R. C., Penzkofer, A., Perazzo, A., Perez, A., Perl, M., Pernicka, M., Perroud, J. -P., Peruzzi, I. M., Pestotnik, R., Peters, K., Peters, M., Petersen, B. A., Petersen, T. C., Petigura, E., Petrak, S., Petrella, A., Petrič, M., Petzold, A., Pia, M. G., Piatenko, T., Piccolo, D., Piccolo, M., Piemontese, L., Piemontese, M., Pierini, M., Pierson, S., Pioppi, M., Piredda, G., Pivk, M., Plaszczynski, S., Polci, F., Pompili, A., Poropat, P., Posocco, M., Potter, C. T., Potter, R. J. L., Prasad, V., Prebys, E., Prencipe, E., Prendki, J., Prepost, R., Prest, M., Prim, M., Pripstein, M., Prudent, X., Pruvot, S., Puccio, E. M. T., Purohit, M. V., Qi, N. D., Quinn, H., Raaf, J., Rabberman, R., Raffaelli, F., Ragghianti, G., Rahatlou, S., Rahimi, A. M., Rahmat, R., Rakitin, A. Y., Randle-Conde, A., Rankin, P., Rashevskaya, I., Ratkovsky, S., Raven, G., Re, V., Reep, M., Regensburger, J. J., Reidy, J., Reif, R., Reisert, B., Renard, C., Renga, F., Ricciardi, S., Richman, J. D., Ritchie, J. L., Ritter, M., Rivetta, C., Rizzo, G., Roat, C., Robbe, P., Roberts, D. A., Robertson, A. I., Robutti, E., Rodier, S., Rodriguez, D. M., Rodriguez, J. L., Rodriguez, R., Roe, N. A., Röhrken, M., Roethel, W., Rolquin, J., Romanov, L., Romosan, A., Ronan, M. T., Rong, G., Ronga, F. J., Roos, L., Root, N., Rosen, M., Rosenberg, E. I., Rossi, A., Rostomyan, A., Rotondo, M., Roussot, E., Roy, J., Rozanska, M., Rozen, Y., Rubin, A. E., Ruddick, W. O., Ruland, A. M., Rybicki, K., Ryd, A., Ryu, S., Ryuko, J., Sabik, S., Sacco, R., Saeed, M. A., Tehrani, F. Safai, Sagawa, H., Sahoo, H., Sahu, S., Saigo, M., Saito, T., Saitoh, S., Sakai, K., Sakamoto, H., Sakaue, H., Saleem, M., Salnikov, A. A., Salvati, E., Salvatore, F., Samuel, A., Sanders, D. A., Sanders, P., Sandilya, S., Sandrelli, F., Sands, W., Sands, W. R., Sanpei, M., Santel, D., Santelj, L., Santoro, V., Santroni, A., Sanuki, T., Sarangi, T. R., Saremi, S., Sarti, A., Sasaki, T., Sasao, N., Satapathy, M., Sato, Nobuhiko, Sato, Noriaki, Sato, Y., Satoyama, N., Satpathy, A., Savinov, V., Savvas, N., Saxton, O. H., Sayeed, K., Schaffner, S. F., Schalk, T., Schenk, S., Schieck, J. R., Schietinger, T., Schilling, C. J., Schindler, R. H., Schmid, S., Schmitz, R. E., Schmuecker, H., Schneider, O., Schnell, G., Schönmeier, P., Schofield, K. C., Schott, G., Schröder, H., Schram, M., Schubert, J., Schümann, J., Schultz, J., Schumm, B. A., Schune, M. H., Schwanke, U., Schwarz, H., Schwiening, J., Schwierz, R., Schwitters, R. F., Sciacca, C., Sciolla, G., Scott, I. J., Seeman, J., Seiden, A., Seitz, R., Seki, T., Sekiya, A. I., Semenov, S., Semmler, D., Sen, S., Senyo, K., Seon, O., Serbo, V. V., Serednyakov, S. I., Serfass, B., Serra, M., Serrano, J., Settai, Y., Seuster, R., Sevior, M. E., Shakhova, K. V., Shang, L., Shapkin, M., Sharma, V., Shebalin, V., Shelkov, V. G., Shen, B. C., Shen, D. Z., Shen, Y. T., Sherwood, D. J., Shibata, T., Shibata, T. A., Shibuya, H., Shidara, T., Shimada, K., Shimoyama, M., Shinomiya, S., Shiu, J. G., Shorthouse, H. W., Shpilinskaya, L. I., Sibidanov, A., Sicard, E., Sidorov, A., Sidorov, V., Siegle, V., Sigamani, M., Simani, M. C., Simard, M., Simi, G., Simon, F., Simonetto, F., Sinev, N. B., Singh, H., Singh, J. B., Sinha, R., Sitt, S., Skovpen, Yu. I., Sloane, R. J., Smerkol, P., Smith, A. J. S., Smith, D., Smith, D. S., Smith, J. G., Smol, A., Snoek, H. L., Snyder, A., So, R. Y., Sobie, R. J., Soderstrom, E., Soha, A., Sohn, Y. S., Sokoloff, M. D., Sokolov, A., Solagna, P., Solovieva, E., Soni, N., Sonnek, P., Sordini, V., Spaan, B., Spanier, S. M., Spencer, E., Speziali, V., Spitznagel, M., Spradlin, P., Staengle, H., Stamen, R., Stanek, M., Stanič, S., Stark, J., Steder, M., Steininger, H., Steinke, M., Stelzer, J., Stevanato, E., Stocchi, A., Stock, R., Stoeck, H., Stoker, D. P., Stroili, R., Strom, D., Strother, P., Strube, J., Stugu, B., Stypula, J., Su, D., Suda, R., Sugahara, R., Sugi, A., Sugimura, T., Sugiyama, A., Suitoh, S., Sullivan, M. K., Sumihama, M., Sumiyoshi, T., Summers, D. J., Sun, L., Sun, S., Sundermann, J. E., Sung, H. F., Susaki, Y., Sutcliffe, P., Suzuki, A., Suzuki, J., Suzuki, J. I., Suzuki, K., Suzuki, S., Suzuki, S. Y., Swain, J. E., Swain, S. K., T'Jampens, S., Tabata, M., Tackmann, K., Tajima, H., Tajima, O., Takahashi, K., Takahashi, S., Takahashi, T., Takasaki, F., Takayama, T., Takita, M., Tamai, K., Tamponi, U., Tamura, N., Tan, N., Tan, P., Tanabe, K., Tanabe, T., Tanaka, H. A., Tanaka, J., Tanaka, M., Tanaka, S., Tanaka, Y., Tanida, K., Taniguchi, N., Taras, P., Tasneem, N., Tatishvili, G., Tatomi, T., Tawada, M., Taylor, F., Taylor, G. N., Taylor, G. P., Telnov, V. I., Teodorescu, L., Ter-Antonyan, R., Teramoto, Y., Teytelman, D., Thérin, G., Thiebaux, Ch., Thiessen, D., Thomas, E. W., Thompson, J. M., Thorne, F., Tian, X. C., Tibbetts, M., Tikhomirov, I., Tinslay, J. S., Tiozzo, G., Tisserand, V., Tocut, V., Toki, W. H., Tomassini, E. W., Tomoto, M., Tomura, T., Torassa, E., Torrence, E., Tosi, S., Touramanis, C., Toussaint, J. C., Tovey, S. N., Trapani, P. P., Treadwell, E., Triggiani, G., Trincaz-Duvoid, S., Trischuk, W., Troost, D., Trunov, A., Tsai, K. L., Tsai, Y. T., Tsujita, Y., Tsukada, K., Tsukamoto, T., Tuggle, J. M., Tumanov, A., Tung, Y. W., Turnbull, L., Turner, J., Turri, M., Uchida, K., Uchida, M., Uchida, Y., Ueki, M., Ueno, K., Ujiie, N., Ulmer, K. A., Unno, Y., Urquijo, P., Ushiroda, Y., Usov, Y., Usseglio, M., Usuki, Y., Uwer, U., Va'vra, J., Vahsen, S. E., Vaitsas, G., Valassi, A., Vallazza, E., Vallereau, A., Vanhoefer, P., van Hoek, W. C., Van Hulse, C., van Winkle, D., Varner, G., Varnes, E. W., Varvell, K. E., Vasileiadis, G., Velikzhanin, Y. S., Verderi, M., Versillé, S., Vervink, K., Viaud, B., Vidal, P. B., Villa, S., Villanueva-Perez, P., Vinograd, E. L., Vitale, L., Vitug, G. M., Voß, C., Voci, C., Voena, C., Volk, A., von Wimmersperg-Toeller, J. H., Vorobyev, V., Vossen, A., Vuagnin, G., Vuosalo, C. O., Wacker, K., Wagner, A. P., Wagner, D. L., Wagner, G., Wagner, M. N., Wagner, S. R., Wagoner, D. E., Walker, D., Walkowiak, W., Wallom, D., Wang, C. C., Wang, C. H., Wang, J., Wang, J. G., Wang, K., Wang, L., Wang, L. L., Wang, P., Wang, T. J., Wang, W. F., Wang, X. L., Wang, Y. F., Wappler, F. R., Watanabe, M., Watson, A. T., Watson, J. E., Watson, N. K., Watt, M., Weatherall, J. H., Weaver, M., Weber, T., Wedd, R., Wei, J. T., Weidemann, A. W., Weinstein, A. J. R., Wenzel, W. A., West, C. A., West, C. G., West, T. J., White, E., White, R. M., Wicht, J., Widhalm, L., Wiechczynski, J., Wienands, U., Wilden, L., Wilder, M., Williams, D. C., Williams, G., Williams, J. C., Williams, K. M., Williams, M. I., Willocq, S. Y., Wilson, J. R., Wilson, M. G., Wilson, R. J., Winklmeier, F., Winstrom, L. O., Winter, M. A., Wisniewski, W. J., Wittgen, M., Wittlin, J., Wittmer, W., Wixted, R., Woch, A., Wogsland, B. J., Wong, Q. K., Wray, B. C., Wren, A. C., Wright, D. M., Wu, C. H., Wu, J., Wu, S. L., Wulsin, H. W., Xella, S. M., Xie, Q. L., Xie, Y., Xu, Z. Z., Yèche, Ch., Yamada, Y., Yamaga, M., Yamaguchi, A., Yamaguchi, H., Yamaki, T., Yamamoto, H., Yamamoto, N., Yamamoto, R. K., Yamamoto, S., Yamanaka, T., Yamaoka, H., Yamaoka, J., Yamaoka, Y., Yamashita, Y., Yamauchi, M., Yan, D. S., Yan, Y., Yanai, H., Yanaka, S., Yang, H., Yang, R., Yang, S., Yarritu, A. K., Yashchenko, S., Yashima, J., Yasin, Z., Yasu, Y., Ye, S. W., Yeh, P., Yi, J. I., Yi, K., Yi, M., Yin, Z. W., Ying, J., Yocky, G., Yokoyama, K., Yokoyama, M., Yokoyama, T., Yoshida, K., Yoshida, M., Yoshimura, Y., Young, C. C., Yu, C. X., Yu, Z., Yuan, C. Z., Yuan, Y., Yumiceva, F. X., Yusa, Y., Yushkov, A. N., Yuta, H., Zacek, V., Zain, S. B., Zallo, A., Zambito, S., Zander, D., Zang, S. L., Zanin, D., Zaslavsky, B. G., Zeng, Q. L., Zghiche, A., Zhang, B., Zhang, J., Zhang, L., Zhang, L. M., Zhang, S. Q., Zhang, Z. P., Zhao, H. W., Zhao, M., Zhao, Z. G., Zheng, Y., Zheng, Y. H., Zheng, Z. P., Zhilich, V., Zhou, P., Zhu, R. Y., Zhu, Y. S., Zhu, Z. M., Zhulanov, V., Ziegler, T., Ziegler, V., Zioulas, G., Zisman, M., Zito, M., Zürcher, D., Zwahlen, N., Zyukova, O., Živko, T., and Žontar, D.

Subjects
High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract

This work is on the Physics of the B Factories. Part A of this book contains a brief description of the SLAC and KEK B Factories as well as their detectors, BaBar and Belle, and data taking related issues. Part B discusses tools and methods used by the experiments in order to obtain results. The results themselves can be found in Part C. Please note that version 3 on the archive is the auxiliary version of the Physics of the B Factories book. This uses the notation alpha, beta, gamma for the angles of the Unitarity Triangle. The nominal version uses the notation phi_1, phi_2 and phi_3. Please cite this work as Eur. Phys. J. C74 (2014) 3026., Comment: 928 pages, version 3 (arXiv:1406.6311v3) corresponds to the alpha, beta, gamma version of the book, the other versions use the phi1, phi2, phi3 notation

Published
2014
Full Text
View/download PDF

8. AzTEC/ASTE 1.1 mm survey of SSA22: Counterpart identification and photometric redshift survey of submillimeter galaxies

Author

Umehata, H., Tamura, Y., Kohno, K., Hatsukade, B., Scott, K. S., Kubo, M., Yamada, T., Ivison, R. J., Cybulski, R., Aretxaga, I., Austermann, J., Hughes, D. H., Ezawa, H., Hayashino, T., Ikarashi, S., Iono, D., Kawabe, R., Matsuda, Y., Matsuo, H., Nakanishi, K., Oshima, T., Perera, T., Takata, T., Wilson, G. W., and Yun, M. S.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present the results from a 1.1 mm imaging survey of the SSA22 field, known for having an overdensity of z=3.1 Lyman-alpha emitting galaxies (LAEs), taken with the AzTEC camera on the Atacama Submillimeter Telescope Experiment (ASTE). We imaged a 950 arcmin$^2$ field down to a 1 sigma sensitivity of 0.7-1.3 mJy/beam to find 125 submillimeter galaxies (SMGs) with a signal to noise ratio >= 3.5. Counterpart identification using radio and near/mid-infrared data was performed and one or more counterpart candidates were found for 59 SMGs. Photometric redshifts based on optical to near-infrared images were evaluated for 45 SMGs of these SMGs with Spitzer/IRAC data, and the median value is found to be z=2.4. By combining these estimation with estimates from the literature we determined that 10 SMGs might lie within the large-scale structure at z=3.1. The two-point angular cross-correlation function between LAEs and SMGs indicates that the positions of the SMGs are correlated with the z=3.1 protocluster. These results suggest that the SMGs were formed and evolved selectively in the high dense environment of the high redshift universe. This picture is consistent with the predictions of the standard model of hierarchical structure formation., Comment: 17 pages, 9 figures, 7 tables, Accepted for publication in MNRAS

Published
2014
Full Text
View/download PDF

9. Investigating the hard X-ray emission from the hottest Abell cluster A2163 with Suzaku

Author

Ota, N., Nagayoshi, K., Pratt, G. W., Kitayama, T., Oshima, T., and Reiprich, T. H.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the results from Suzaku observations of the hottest Abell galaxy cluster A2163 at $z=0.2$. To study the physics of gas heating in cluster mergers, we investigated hard X-ray emission from the merging cluster A2163, which hosts the brightest synchrotron radio halo. We analyzed hard X-ray spectra accumulated from two-pointed Suzaku observations. Non-thermal hard X-ray emission should result from the inverse Compton (IC) scattering of relativistic electrons by the CMB photons. To measure this emission, the dominant thermal emission in the hard X-ray band must be modeled in detail. To this end, we analyzed the combined broad-band X-ray data of A2163 collected by Suzaku and XMM-Newton, assuming single- and multi-temperature models for thermal emission and the power-law model for non-thermal emission. From the Suzaku data, we detected significant hard X-ray emission from A2163 in the 12-60 keV band at the $28\sigma$ level (or at the $5.5\sigma$ level if a systematic error is considered). The Suzaku HXD spectrum alone is consistent with the single-T thermal model of gas temperature $kT=14$ keV. From the XMM data, we constructed a multi-T model including a very hot ($kT=18$ keV) component in the NE region. Incorporating the multi-T and the power-law models into a two-component model with a radio-band photon index, the 12-60 keV energy flux of non-thermal emission is constrained within $5.3 \pm 0.9 (\pm 3.8)\times 10^{-12}~{\rm erg\, s^{-1} cm^{-2}}$. The 90% upper limit of detected IC emission is marginal ($< 1.2\times 10^{-11}~{\rm erg\, s^{-1} cm^{-2}}$ in the 12-60 keV). The estimated magnetic field in A2163 is $B > 0.098~{\rm \mu G}$. While the present results represent a three-fold increase in the accuracy of the broad band spectral model of A2163, more sensitive hard X-ray observations are needed to decisively test for the presence of hard X-ray emission due to IC emission., Comment: 7 pages, 7 figures, A&A accepted. Minor correction

Published
2013
Full Text
View/download PDF

10. Mucin expression in gastric- and gastro-oesophageal signet-ring cell cancer: results from a comprehensive literature review and a large cohort study of Caucasian and Asian gastric cancer

Author

Kerckhoffs, K. G. P., Liu, D. H. W., Saragoni, L., van der Post, R. S., Langer, R., Bencivenga, M., Iglesias, M., Gallo, G., Hewitt, L. C., Fazzi, G. E., Vos, A. M., Renaud, F., Yoshikawa, T., Oshima, T., Tomezzoli, A., de Manzoni, G., Arai, T., Kushima, R., Carneiro, F., and Grabsch, H. I.

Published
2020
Full Text
View/download PDF

11. The source counts of submillimetre galaxies detected at 1.1 mm

Author

Scott, K. S., Wilson, G. W., Aretxaga, I., Austermann, J. E., Chapin, E. L., Dunlop, J. S., Ezawa, H., Halpern, M., Hatsukade, B., Hughes, D. H., Kawabe, R., Kim, S., Kohno, K., Lowenthal, J. D., Montana, A., Nakanishi, K., Oshima, T., Sanders, D., Scott, D., Scoville, N., Tamura, Y., Welch, D., Yun, M. S., and Zeballos, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The source counts of galaxies discovered at sub-millimetre and millimetre wavelengths provide important information on the evolution of infrared-bright galaxies. We combine the data from six blank-field surveys carried out at 1.1 mm with AzTEC, totalling 1.6 square degrees in area with root-mean-square depths ranging from 0.4 to 1.7 mJy, and derive the strongest constraints to date on the 1.1 mm source counts at flux densities S(1100) = 1-12 mJy. Using additional data from the AzTEC Cluster Environment Survey to extend the counts to S(1100) ~ 20 mJy, we see tentative evidence for an enhancement relative to the exponential drop in the counts at S(1100) ~ 13 mJy and a smooth connection to the bright source counts at >20 mJy measured by the South Pole Telescope; this excess may be due to strong lensing effects. We compare these counts to predictions from several semi-analytical and phenomenological models and find that for most the agreement is quite good at flux densities > 4 mJy; however, we find significant discrepancies (>3sigma) between the models and the observed 1.1 mm counts at lower flux densities, and none of them are consistent with the observed turnover in the Euclidean-normalised counts at S(1100) < 2 mJy. Our new results therefore may require modifications to existing evolutionary models for low luminosity galaxies. Alternatively, the discrepancy between the measured counts at the faint end and predictions from phenomenological models could arise from limited knowledge of the spectral energy distributions of faint galaxies in the local Universe., Comment: 16 pages, 3 figures, 4 tables; accepted for publication in MNRAS

Published
2012
Full Text
View/download PDF

12. Deep 1.1 mm-wavelength imaging of the GOODS-South field by AzTEC/ASTE -- II. Redshift distribution and nature of the submillimetre galaxy population

Author

Yun, Min S., Scott, K. S., Guo, Yicheng, Aretxaga, I., Giavalisco, M., Austermann, J. E., Capak, P., Chen, Yuxi, Ezawa, H., Hatsukade, B., Hughes, D. H., Iono, D., Johnson, S., Kawabe, R., Kohno, K., Lowenthal, J., Miller, N., Morrison, G., Oshima, T., Perera, T. A., Salvato, M., Silverman, J., Tamura, Y., Williams, C. C., and Wilson, G. W.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the results of the counterpart identification and a detailed analysis of the physical properties of the 48 sources discovered in our deep 1.1mm wavelength imaging survey of the GOODS-South field using the AzTEC instrument on the Atacama Submillimeter Telescope Experiment (ASTE). One or more robust or tentative counterpart candidate is found for 27 and 14 AzTEC sources, respectively, by employing deep radio continuum, Spitzer MIPS & IRAC, and LABOCA 870 micron data. Five of the sources (10%) have two robust counterparts each, supporting the idea that these galaxies are strongly clustered and/or heavily confused. Photometric redshifts and star formation rates (SFRs) are derived by analyzing UV-to-optical and IR-to-radio SEDs. The median redshift of z~2.6 is similar to other earlier estimates, but we show that 80% of the AzTEC-GOODS sources are at z>2, with a significant high redshift tail (20% at z>3.3). Rest-frame UV and optical properties of AzTEC sources are extremely diverse, spanning 10 magnitude in the i- and K-band photometry with median values of i=25.3 and K=22.6 and a broad range of red colour (i-K=0-6). These AzTEC sources are some of the most luminous galaxies in the rest-frame optical bands at z>2, with inferred stellar masses of (1-30) x 10^{10} solar masses and UV-derived star formation rates of SFR(UV) > 10-1000 solar masses per year. The IR-derived SFR, 200-2000 solar masses per year, is independent of redshift or stellar mass. The resulting specific star formation rates, SSFR = 1-100 per Gyr, are 10-100 times higher than similar mass galaxies at z=0, and they extend the previously observed rapid rise in the SSFR with redshift to z=2-5. These galaxies have a SFR high enough to have built up their entire stellar mass within their Hubble time. We find only marginal evidence for an AGN contribution to the near-IR and mid-IR SEDs. (abridged), Comment: 31 pages including 14 figures, accepted for publication in the MNRAS. A higher quality Figure 1 is also included as Figure1.jpg

Published
2011
Full Text
View/download PDF

13. AzTEC millimeter survey of the COSMOS field - III. Source catalog over 0.72 sq. deg. and plausible boosting by large-scale structure

Author

Aretxaga, I., Wilson, G. W., Aguilar, E., Alberts, S., Scott, K. S., Scoville, N., Yun, M. S., Austermann, J., Downes, T. P., Ezawa, H., Hatsukade, B., Hughes, D. H., Kawabe, R., Kohno, K., Oshima, T., Perera, T. A., Tamura, Y., and Zeballos, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a 0.72 sq. deg. contiguous 1.1mm survey in the central area of the COSMOS field carried out to a 1sigma ~ 1.26 mJy/beam depth with the AzTEC camera mounted on the 10m Atacama Submillimeter Telescope Experiment (ASTE). We have uncovered 189 candidate sources at a signal-to-noise ratio S/N >= 3.5, out of which 129, with S/N >= 4, can be considered to have little chance of being spurious (< 2 per cent). We present the number counts derived with this survey, which show a significant excess of sources when compared to the number counts derived from the ~0.5 sq. deg. area sampled at similar depths in the Scuba HAlf Degree Extragalactic Survey (SHADES, Austermann et al. 2010). They are, however, consistent with those derived from fields that were considered too small to characterize the overall blank-field population. We identify differences to be more significant in the S > 5 mJy regime, and demonstrate that these excesses in number counts are related to the areas where galaxies at redshifts z < 1.1 are more densely clustered. The positions of optical-IR galaxies in the redshift interval 0.6 < z < 0.75 are the ones that show the strongest correlation with the positions of the 1.1mm bright population (S > 5 mJy), a result which does not depend exclusively on the presence of rich clusters within the survey sampled area. The most likely explanation for the observed excess in number counts at 1.1mm is galaxy-galaxy and galaxy-group lensing at moderate amplification levels, that increases in amplitude as one samples larger and larger flux densities. This effect should also be detectable in other high redshift populations., Comment: 21 pages, 17 figures, accepted for publication in MNRAS

Published
2011
Full Text
View/download PDF

14. AzTEC/ASTE 1.1-mm Survey of the AKARI Deep Field South: source catalogue and number counts

Author

Hatsukade, B., Kohno, K., Aretxaga, I., Austermann, J. E., Ezawa, H., Hughes, D. H., Ikarashi, S., Iono, D., Kawabe, R., Khan, S., Matsuo, H., Matsuura, S., Nakanishi, K., Oshima, T., Perera, T., Scott, K. S., Shirahata, M., Takeuchi, T. T., Tamura, Y., Tanaka, K., Tosaki, T., Wilson, G. W., and Yun, M. S.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present results of a 1.1 mm deep survey of the AKARI Deep Field South (ADF-S) with AzTEC mounted on the Atacama Submillimetre Telescope Experiment (ASTE). We obtained a map of 0.25 sq. deg area with an rms noise level of 0.32-0.71 mJy. This is one of the deepest and widest maps thus far at millimetre and submillimetre wavelengths. We uncovered 198 sources with a significance of 3.5-15.6 sigma, providing the largest catalog of 1.1 mm sources in a contiguous region. Most of the sources are not detected in the far-infrared bands of the AKARI satellite, suggesting that they are mostly at z ~ 1.5 given the detection limits. We constructed differential and cumulative number counts in the ADF-S, the Subaru/XMM Newton Deep Field (SXDF), and the SSA 22 field surveyed by AzTEC/ASTE, which provide currently the tightest constraints on the faint end. The integration of the best-fit number counts in the ADF-S find that the contribution of 1.1 mm sources with fluxes >=1 mJy to the cosmic infrared background (CIB) at 1.1 mm is 12-16%, suggesting that the large fraction of the CIB originates from faint sources of which the number counts are not yet constrained. We estimate the cosmic star-formation rate density contributed by 1.1 mm sources with >=1 mJy using the best-fit number counts in the ADF-S and find that it is lower by about a factor of 5-10 compared to those derived from UV/optically-selected galaxies at z ~ 2-3. The fraction of stellar mass of the present-day universe produced by 1.1 mm sources with >=1 mJy at z >= 1 is ~20%, calculated by the time integration of the star-formation rate density. If we consider the recycled fraction of >0.4, which is the fraction of materials forming stars returned to the interstellar medium, the fraction of stellar mass produced by 1.1 mm sources decrease to <~10%., Comment: 15 pages, 12 figure, accepted for publication in MNRAS

Published
2010
Full Text
View/download PDF

15. Deep 1.1 mm-wavelength imaging of the GOODS-S field by AzTEC/ASTE - I. Source catalogue and number counts

Author

Scott, K. S., Yun, M. S., Wilson, G. W., Austermann, J. E., Aguilar, E., Aretxaga, I., Ezawa, H., Ferrusca, D., Hatsukade, B., Hughes, D. H., Iono, D., Giavalisco, M., Kawabe, R., Kohno, K., Mauskopf, P. D., Oshima, T., Perera, T. A., Rand, J., Tamura, Y., Tosaki, T., Velazquez, M., Williams, C. C., and Zeballos, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged] We present the first results from a 1.1 mm confusion-limited map of the GOODS-S field taken with AzTEC on the ASTE telescope. We imaged a 270 sq. arcmin field to a 1\sigma depth of 0.48 - 0.73 mJy/beam, making this one of the deepest blank-field surveys at mm-wavelengths ever achieved. Although our GOODS-S map is extremely confused, we demonstrate that our source identification and number counts analyses are robust, and the techniques discussed in this paper are relevant for other deeply confused surveys. We find a total of 41 dusty starburst galaxies with S/N >= 3.5 within this uniformly covered region, where only two are expected to be false detections. We derive the 1.1mm number counts from this field using both a "P(d)" analysis and a semi-Bayesian technique, and find that both methods give consistent results. Our data are well-fit by a Schechter function model with (S', N(3mJy), \alpha) = (1.30+0.19 mJy, 160+27 (mJy/deg^2)^(-1), -2.0). Given the depth of this survey, we put the first tight constraints on the 1.1 mm number counts at S(1.1mm) = 0.5 mJy, and we find evidence that the faint-end of the number counts at S(850\mu m) < 2.0 mJy from various SCUBA surveys towards lensing clusters are biased high. In contrast to the 870 \mu m survey of this field with the LABOCA camera, we find no apparent under-density of sources compared to previous surveys at 1.1 mm. Additionally, we find a significant number of SMGs not identified in the LABOCA catalogue. We find that in contrast to observations at wavelengths < 500 \mu m, MIPS 24 \mu m sources do not resolve the total energy density in the cosmic infrared background at 1.1 mm, demonstrating that a population of z > 3 dust-obscured galaxies that are unaccounted for at these shorter wavelengths potentially contribute to a large fraction (~2/3) of the infrared background at 1.1 mm., Comment: 21 pages, 9 figures. Accepted to MNRAS.

Published
2010
Full Text
View/download PDF

16. A Comparison of Measurement Equivalence Methods Based on Confirmatory Factor Analysis and Item Response Theory.

Author

Flowers, Claudia P., Raju, Nambury S., and Oshima, T. C.

Abstract

Current interest in the assessment of measurement equivalence emphasizes two methods of analysis, linear, and nonlinear procedures. This study simulated data using the graded response model to examine the performance of linear (confirmatory factor analysis or CFA) and nonlinear (item-response-theory-based differential item function or IRT-Based DIF) methods. Two CFA procedures, lambda (slope) structure only and lambda and tau (slope and intercept) structures, were used to examine measurement equivalence across focal and reference groups. An IRT-based, noncompensatory DIF (NC-DIF) procedure (N. Raju, W. van der Linden, and P. Fleer, 1995) was also used to examine measurement equivalence across groups. Results indicate that the lambda procedure successfully identified items that had differences in the alpha-parameters, but did not identify items that had differences in the beta-parameters. The lambda/tau and NC-DIF procedures identified items that had differences in the beta-parameters. The lambda-tau and NC-DIF procedures were not, however, as sensitive to items that had differences only in the alpha-parameters. When the focal and reference groups had different ability distributions (or impact), the lambda/tau procedure had a lower (or an acceptable) Type II error rate (in detecting true positives), but had a much higher (or an unacceptable) Type I error rate (in detecting false positives). The NC-DIF procedure appeared to have acceptable Type I and Type II error rates in both no-impact and impact scenarios. (Contains 5 tables and 23 references.) (Author/SLD)

Published
2002

17. Suzaku broad-band spectroscopy of RX J1347.5-1145: constraints on the extremely hot gas and non-thermal emission

Author

Ota, N., Murase, K., Kitayama, T., Komatsu, E., Hattori, M., Matsuo, H., Oshima, T., Suto, Y., and Yoshikawa, K.

Subjects
Astrophysics
Abstract

We present the results from the analysis of long Suzaku observations of the most X-ray luminous galaxy cluster RX J1347.5-1145 at z=0.451. Aims: We study physical properties of the hot (~20 keV) gas clump in the south-east (SE) region discovered by the Sunyaev-Zel'dovich (SZ) effect observations, to understand the gas physics of a violent cluster merger. We also explore a signature of non-thermal emission using the hard X-ray data. Results: We find that the single-temperature model fails to reproduce the continuum emission and Fe-K lines measured by XIS simultaneously. The two-temperature model with a very hot component improves the fit, although the XIS data can only give a lower bound on its temperature. We detect the hard X-ray emission in the 12-40 keV band at the 7 sigma level; however, the significance becomes marginal when the systematic error in the background estimation is included. With the Suzaku + Chandra joint analysis, we determine the temperature of the SE excess component to be 25.3^{+6.1}_{-4.5} ^{+6.9}_{-9.5} keV (90% statistical and systematic errors), which is in an excellent agreement with the previous SZ + X-ray analysis. This is the first time that the X-ray spectroscopy alone gives a good measurement of the temperature of the hot component in the SE region, which is made possible by Suzaku's unprecedented sensitivity to the wide X-ray band. These results strongly indicate that the cluster has undergone a recent, violent merger. The spectral analysis shows that the SE component is consistent with being thermal. We find the 3 sigma upper limit on the non-thermal flux, F < 8e-12 erg s^{-1} cm^{-2} in the 12-60 keV band. Combining this limit with a recent discovery of the radio mini halo at 1.4 GHz, we find a lower limit on the strength of the intracluster magnetic field, B > 0.007 micro G., Comment: 15 pages, 13 figures. Accepted for publication in A&A

Published
2008
Full Text
View/download PDF

18. A bright, dust-obscured, millimeter-selected galaxy beyond the Bullet Cluster (1E0657-56)

Author

Wilson, G. W., Hughes, D., Aretxaga, I., Ezawa, H., Austermann, J. E., Doyle, S., Ferrusca, D., Hernandez-Curiel, I., Kawabe, R., Kitayama, T., Kohno, K., Kuboi, A., Matsuo, H., Mauskopf, P. D., Murakoshi, Y., Montana, A., Natarajan, P., Oshima, T., Ota, N., Perera, T., Rand, J., Scott, K. S., Tanaka, K., Tsuboi, M., Williams, C. C., Yamaguchi, N., and Yun, M. S.

Subjects
Astrophysics
Abstract

Deep 1.1 mm continuum observations of 1E0657-56 (the "Bullet Cluster") taken with the millimeter-wavelength camera AzTEC on the 10-m Atacama Submillimeter Telescope Experiment (ASTE), have revealed an extremely bright (S$_{\rm{1.1mm}}=15.9$ mJy) unresolved source. This source, MMJ065837-5557.0, lies close to a maximum in the density of underlying mass-distribution, towards the larger of the two interacting clusters as traced by the weak-lensing analysis of Clowe et al. 2006. Using optical--IR colours we argue that MMJ065837-5557.0 lies at a redshift of $z = 2.7 \pm 0.2$. A lensing-derived mass-model for the Bullet Cluster shows a critical-line (caustic) of magnification within a few arcsecs of the AzTEC source, sufficient to amplify the intrinsic millimeter-wavelength flux of the AzTEC galaxy by a factor of $\gg 20$. After subtraction of the foreground cluster emission at 1.1mm due to the Sunyaev-Zel'dovich effect, and correcting for the magnification, the rest-frame FIR luminosity of MMJ065837-5557.0 is $\le 10^{12} \rm L_{\odot}$, characteristic of a luminous infrared galaxy (LIRG). We explore various scenarios to explain the colors, morphologies and positional offsets between the potential optical and IR counterparts, and their relationship with MMJ065837-5557.0. Until higher-resolution and more sensitive (sub)millimeter observations are available, the detection of background galaxies close to the caustics of massive lensing clusters offers the only opportunity to study this intrinsically faint millimeter-galaxy population., Comment: 11 pages, 7 figures, accepted by MNRAS

Published
2008

19. Status of the ITER remote experimentation centre

Author

Farthing, J., Ozeki, T., Clement Lorenzo, S., Nakajima, N., Sartori, F., De Tommasi, G., Manduchi, G., Barbato, P., Rigoni, A., Vitale, V., Giruzzi, G., Mattei, M., Mele, A., Imbeaux, F., Artaud, J.-F., Robin, F., Noe, J., Joffrin, E., Hynes, A., Hemming, O., Wheatley, M., O’hira, S., Ide, S., Ishii, Y., Matsukawa, M., Kubo, H., Totsuka, T., Urano, H., Naito, O., Hayashi, N., Miyata, Y., Namekawa, M., Wakasa, A., Oshima, T., Nakanishi, H., and Yamanaka, K.

Published
2018
Full Text
View/download PDF

20. Effect of Purification Procedures on DIF Analysis in IRTPRO

Author

Fikis, David R. J. and Oshima, T. C.

Abstract

Purification of the test has been a well-accepted procedure in enhancing the performance of tests for differential item functioning (DIF). As defined by Lord, purification requires reestimation of ability parameters after removing DIF items before conducting the final DIF analysis. IRTPRO 3 is a recently updated program for analyses in item response theory, with built-in DIF tests but not purification procedures. A simulation study was conducted to investigate the effect of two new methods of purification. The results suggested that one of the purification procedures showed significantly improved power and Type I error. The procedure, which can be cumbersome by hand, can be easily applied by practitioners by using the web-based program developed for this study.

Published
2017
Full Text
View/download PDF

21. Differential Item Functioning and Language Translation: A Cross-National Study with a Test Developed for Certification.

Author

Price, Larry R. and Oshima, T. C.

Abstract

Often, educational and psychological measurement instruments must be translated from one language to another when they are administered to different cultural groups. The translation process often necessarily introduces measurement inequivalence. Therefore, an examination may be said to exhibit differential functioning if the test provides a consistent advantage to one particular race or culture through the manner in which the test items are written. One thousand American and 1,134 Japanese entry-level examinees participating in a scuba diving certification course took a standardized criterion mastery test for certification. The parametric framework Differential Functioning of Items and Tests (DFIT) proposed by N. Raju, W. van der Linden, and P. Fleer (1992) was used to detect differential item functioning (DIF). Out of a total of 30 items, 10 were found to exhibit significant noncompensatory DIF. Differential test functioning was also found to be significant. This paper demonstrates that the new DFIT technique can be applied successfully to the translated data, and that possible causes for the differential functioning can be examined using results from the DFIT analysis. (Contains 3 figures, 5 tables, and 25 references.) (Author/SLD)

Published
1998

22. Detection of an Iron Emission Feature from the Lensed BAL QSO H1413+117 at z=2.56

Author

Oshima, T., Mitsuda, K., Fujimoto, R., Iyomoto, N., Futamoto, K., Hattori, M., Ota, N., Mori, K., Ikebe, Y., Miralles, J. M., and Kneib, J-P.

Subjects
Astrophysics
Abstract

We present the X-ray energy spectrum of the lensed BAL QSO H1413+117 (the Cloverleaf) at z=2.56 observed with the Chandra X-ray observatory. We detected 293 photons in a 40 ks Advanced CCD Imaging Spectrometer (ACIS-S) observation. The X-ray image consists of four lensed image components, thus the photons are from the lensed QSO itself. The overall spectrum can be described with a power-law function heavily absorbed by neutral matter at a redshift consistent with the QSO redshift. This supports the idea that intrinsic absorption is significant for BAL QSOs. The spectral fit significantly (99% confidence) improves when we include an emission line. The centroid energy and intrinsic width (Gaussian \sigma) of the line are 6.21 \pm 0.16 keV and 220 ^{+270}_{-130} eV (90% errors), respectively, in the QSO rest frame, assuming the absorbed power-law as the continuum. The equivalent width of the line in the QSO rest frame is 960 ^{+1400}_{-480} eV. We suggest that the large equivalent width, the centroid energy, and the line broadness can be explained by iron K emission arising from X-ray reprocessing in the BAL flow, assuming it has a conical thin-sheet structure., Comment: 3 figures, Accepted for publication in ApJ Letters

Published
2001
Full Text
View/download PDF

23. The Consistency of DIF/DTF across Different Test Administrations: A Multidimensional Perspective.

Author

Flowers, Claudia P. and Oshima, T. C.

Abstract

This study was patterned after a previous study by Skaggs and Lissitz (1992) in which inconsistency of differential item functioning (DIF) was reported across test administrations. They suggested multidimensionality of test data as one possible reason for inconsistency. Therefore, in this study, DIF indices which were developed recently with a multidimensional perspective were included. In addition, the consistency of differential test functioning (DTF) was evaluated. DIF/DTF analyses were conducted for both gender and ethnic differences. Ten random samples of 1,000 examinees from each gender and ethnic category were taken from a math basic skills test which was administered in a statewide testing program in two separate years (1984 and 1987). In general, results indicated a more favorable evaluation of the consistency of DIF indices than the Skaggs and Lissitz study. Possible reasons for conflicting conclusions are discussed. (Contains 18 references and 9 tables.) (Author/SLD)

Published
1994

24. Evaluation of Procedures for Linking Multidimensional Item Calibrations.

Author

Oshima, T. C. and Davey, T. C.

Abstract

This paper evaluated multidimensional linking procedures with which multidimensional test data from two separate calibrations were put on a common scale. Data were simulated with known ability distributions varying on two factors which made linking necessary: mean vector differences and variance-covariance (v-c) matrix differences. After the calibrations of multidimensional item parameters, blocks of means from item parameter estimates were used to equate the two groups. The linking was effective for mean vector differences. The linking for v-c matrix differences was less effective, but encouraging. Suggestions for future research are provided. Four tables are attached. (Contains 6 references.) (Author)

Published
1994

25. Differential Item Functioning with a Criterion-Referenced Test: Use of Limited Closed-Interval Measures.

Author

Oshima, T. C.

Abstract

The purpose of this study was to introduce a procedure to detect differential item functioning (DIF) particularly suitable for criterion-referenced tests and to demonstrate how this approach would affect the identification of DIF items using real data sets. The procedure based on item response theory (IRT) assesses DIF at a limited closed interval of thetas at which a cutoff score fails. Illustrative data showed that identification of DIF could be quite different with this unconventional procedure as opposed to traditional DIF measures with which DIF was assessed over the entire range of ability. It was recommended that test development practitioners be actively involved in the DIF analysis to investigate not only if an item is biased, but where it may be biased. Three figures, and five tables are included. (Contains 8 references.) (Author)

Published
1993

26. Evaluation of DTF and DIF in Two-Dimensional IRT.

Author

Oshima, T. C.

Abstract

In 1992 N. S. Raju and others proposed a general procedure for assessing differential test functioning (DTF) and item bias (differential item functioning or DIF) in tests developed with unidimensional, multidimensional, or polytomous item response theory (IRT) models. The purpose of this paper is to assess the adequacy and validity of their technique in the two-dimensional IRT setup. Following Raju and others, a chi square test is described for determining whether or not an observed DTF is significantly different from zero. When an observed DTF is statistically significant, one may begin the search for items that may be causing the significant chi square. After deletion of items with a high positive compensatory DIF, the DTF index and its chi square should be recomputed. The technique is illustrated with generated 40-item two-dimensional data sets. Once the multidimensional item parameters are given and differences in item parameters between the reference and focal groups are found, the new procedure identifies DTF and DIF as expected. Five tables present analysis results. (Contains 15 references.) (SLD)

Published
1993

27. A faster and more reliable data acquisition system for the full performance of the SciCRT

Author

Sasai, Y., Matsubara, Y., Itow, Y., Sako, T., Kawabata, T., Lopez, D., Hikimochi, R., Tsuchiya, A., Ikeno, M., Uchida, T., Tanaka, M., Munakata, K., Kato, C., Nakamura, Y., Oshima, T., Koike, T., Kozai, M., Shibata, S., Oshima, A., Takamaru, H., Kojima, H., Tsuchiya, H., Watanabe, K., Koi, T., Valdés-Galicia, J.F., Ortiz, E., Musalem, O., Hurtado, A., Garcia, R., Anzorena, M., Taylor, R., Barrantes, M., and González, L.X.

Published
2017
Full Text
View/download PDF

32. An Effect Size Measure for Raju's Differential Functioning for Items and Tests

Author

Wright, Keith D. and Oshima, T. C.

Abstract

This study established an effect size measure for differential functioning for items and tests' noncompensatory differential item functioning (NCDIF). The Mantel-Haenszel parameter served as the benchmark for developing NCDIF's effect size measure for reporting moderate and large differential item functioning in test items. The effect size of NCDIF is influenced by the model, the discrimination parameter, and the difficulty parameter. Therefore, tables of NCDIF's effect size were presented at given levels of "a," "b," and "c" parameters. In addition, a general effect size recommendation for moderate and large NCDIF is also established.

Published
2015
Full Text
View/download PDF

33. Multiple-Group Noncompensatory Differential Item Functioning in Raju's Differential Functioning of Items and Tests

Author

Oshima, T. C., Wright, Keith, and White, Nick

Abstract

Raju, van der Linden, and Fleer (1995) introduced a framework for differential functioning of items and tests (DFIT) for unidimensional dichotomous models. Since then, DFIT has been shown to be a quite versatile framework as it can handle polytomous as well as multidimensional models both at the item and test levels. However, DFIT is still limited by the two-group comparison (reference vs. focal group). In real testing situations, it is quite common that a practitioner or researcher may want to compare more than two groups simultaneously. Ethnicity, for example, may have three or more categories. This current study extends the two-group noncompensatory differential item functioning index (NCDIF) in DFIT to multiple-group NCDIF. The significance test developed for the two-group NCDIF and effect size were utilized in the multiple-group cases. The effectiveness of this new approach is demonstrated in a simulation study where various degrees and types of DIF are embedded.

Published
2015
Full Text
View/download PDF

40. 1451P Neoadjuvant and adjuvant pembrolizumab (pembro) + chemotherapy (chemo) for locally advanced gastric or gastroesophageal junction (G/GEJ) cancer: Patient-reported outcomes (PROs) from the phase III KEYNOTE-585 study

Author

Shitara, K., Rha, S.Y., Wyrwicz, L.S., Oshima, T., Karaseva, N., Osipov, M., Yasui, H., Yabusaki, H., Afanasyev, S., Park, Y-K., Al-Batran, S-E., Yoshikawa, T., Yanez Weber, P.E., Di Bartolomeo, M., Lonardi, S., Guan, Y., Valderrama, A., Shih, C-S., Fang, X., and Bang, Y-J.

Published
2024
Full Text
View/download PDF

41. Effect of Multiple Testing Adjustment in Differential Item Functioning Detection

Author

Kim, Jihye and Oshima, T. C.

Abstract

In a typical differential item functioning (DIF) analysis, a significance test is conducted for each item. As a test consists of multiple items, such multiple testing may increase the possibility of making a Type I error at least once. The goal of this study was to investigate how to control a Type I error rate and power using adjustment procedures for multiple testing, which have been widely used in applied statistics. In the simulation, four distinct DIF methods were performed under various testing conditions. The methods were the Mantel-Haenszel (MH) method, the logistic regression (LR) procedure, the Differential Functioning Item and Test (DFIT) framework, and Lord's chi-square test. As an adjustment procedure, the Bonferroni correction, Holm's procedure, or the Benjamini and Hochberg (BH) false discovery rate was applied. The results showed the MH and the LR clearly benefited from Holm's and the BH adjustments, whereas the DFIT and Lord's chi-square test did not require adjustments for conditions under this study. (Contains 2 tables.)

Published
2013
Full Text
View/download PDF

42. Student Mobility and Its Implication for Schools' Adequate Yearly Progress

Author

Thompson, Sharon M., Meyers, Joel, and Oshima, T. Chris

Abstract

Correlation and regression analyses were used to investigate the relationship of student mobility (as expressed by the school-level mobility rate) and first through fifth grade reading, language arts, and mathematics achievement for a statewide sample of 1062 elementary schools. Comparison data were analyzed to further investigate the relationship of school-level mobility rate and achievement for schools that met adequate yearly progress (AYP), a mandate of the No Child Left Behind Act of 2001, and those that did not meet AYP, Findings indicated moderate, negative correlations between mobility rate and achievement across grade levels and subject areas; modest, negative correlations between achievement and mobility when school enrollment size or school poverty status were controlled; and, no significant differences in mobility rate, school size and poverty status for schools th at met AYP when compared to schools that did not meet AYP. (Contains 4 tables.)

Published
2011

46. A Comparison of Unidimensional and Three-Dimensional Differential Item Functioning Analysis Using Two-Dimensional Data

Author

Snow, Teresa K. and Oshima, T. C.

Abstract

Oshima, Raju, and Flowers demonstrated the use of an item response theory-based technique for analyzing differential item function (DIF) and differential test function for dichotomously scored data that are intended to be multidimensional. Their study assumed that the number of intended-to-be measured dimensions was correctly identified. In practice, however, the number of dimensions may be misidentified. Therefore, the purpose of this study was to demonstrate the effects of both underestimation and overestimation of the number of intended-to-be measured dimensions on the multidimensional DIF analysis using simulated two-dimensional data with known DIF items. Results show that overestimation of the number of y traits had a consequence of decreased power. Underestimation resulted in missing a certain type of nonuniform DIF, as well as confounding the impact with DIF. Recommendations are made on how to conduct a DIF investigation with a multidimensional within-item test. (Contains 2 figures and 5 tables.)

Published
2009
Full Text
View/download PDF

47. Raju's Differential Functioning of Items and Tests (DFIT)

Author

Oshima, T. C. and Morris, S. B.

Abstract

Nambury S. Raju (1937-2005) developed two model-based indices for differential item functioning (DIF) during his prolific career in psychometrics. Both methods, Raju's area measures (Raju, 1988) and Raju's DFIT (Raju, van der Linden, & Fleer, 1995), are based on quantifying the gap between item characteristic functions (ICFs). This approach provides an intuitive and flexible methodology for assessing DIF. The purpose of this tutorial is to explain DFIT and show how this methodology can be utilized in a variety of DIF applications.

Published
2008
Full Text
View/download PDF

48. Identifying Possible Sources of Differential Functioning Using Differential Bundle Functioning with Polytomously Scored Data

Author

McCarty, F. A., Oshima, T. C., and Raju, Nambury S.

Abstract

Oshima, Raju, Flowers, and Slinde (1998) described procedures for identifying sources of differential functioning for dichotomous data using differential bundle functioning (DBF) derived from the differential functioning of items and test (DFIT) framework (Raju, van der Linden, & Fleer, 1995). The purpose of this study was to extend the procedures for dichotomous DBF to the polytomous case and to illustrate how DBF analysis can be conducted with polytomous scoring, common to psychological and educational rating scales. The data set used was parent and teacher ratings of child problem behaviors. Three group contrasts (teacher vs. parent, boy vs. girl, and random groups) and two bundle organizing principles (subscale designation and random selection) were used for the DBF analysis. Interpretations of bundle indexes in the context of child problem behaviors were presented.

Published
2007
Full Text
View/download PDF

49. Standardized Conditional 'SEM': A Case for Conditional Reliability

Author

Raju, Nambury S., Price, Larry R., Oshima, T. C., and Nering, Michael L.

Abstract

An examinee-level (or conditional) reliability is proposed for use in both classical test theory (CTT) and item response theory (IRT). The well-known group-level reliability is shown to be the average of conditional reliabilities of examinees in a group or a population. This relationship is similar to the known relationship between the square of the conditional standard error of measurement ("SEM") and the square of the group-level "SEM". The proposed conditional reliability is illustrated with an empirical data set in the CTT and IRT frameworks. (Contains 3 tables.)

Published
2007
Full Text
View/download PDF

50. A New Method for Assessing the Statistical Significance in the Differential Functioning of Items and Tests (DFIT) Framework

Author

Oshima, T. C., Raju, Nambury S., and Nanda, Alice O.

Abstract

A new item parameter replication method is proposed for assessing the statistical significance of the noncompensatory differential item functioning (NCDIF) index associated with the differential functioning of items and tests framework. In this new method, a cutoff score for each item is determined by obtaining a (1-alpha ) percentile rank score from a frequency distribution of NCDIF values under the no-DIF condition by generating a large number of item parameters based on the item parameter estimates and their variance-covariance structures from a computer program such as BIILOG-MG3. This cutoff for each item can be used as the basis for determining whether a given NCDIF index is significantly different from zero. This new method has definite advantages over the current method and yields cutoff values that are tailored to a particular data set and a particular item. A Monte Carlo assessment of this new method is presented and discussed.

Published
2006
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results