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3,143 results on '"Corcoran, M"'

1. Discovery of extraordinary X-ray emission from magnetospheric interaction in the unique binary stellar system $\epsilon$ Lupi

Author: Das, B., Petit, V., Nazé, Y., Corcoran, M. F., Cohen, D. H., Biswas, A., Chandra, P., David-Uraz, A., Leutenegger, M. A., Neiner, C., Pablo, H., Paunzen, E., Shultz, M. E., ud-Doula, A., and Wade, G. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report detailed X-ray observations of the unique binary system $\epsilon$ Lupi, the only known short-period binary consisting of two magnetic early-type stars. The components have comparably strong, but anti-aligned magnetic fields. The orbital and magnetic properties of the system imply that the magnetospheres overlap at all orbital phases, suggesting the possibility of variable inter-star magnetospheric interaction due to the non-negligible eccentricity of the orbit. To investigate this effect, we observed the X-ray emission from $\epsilon$ Lupi both near and away from periastron passage, using the Neutron Star Interior Composition Explorer mission (NICER) X-ray Telescope. We find that the system produces excess X-ray emission at the periastron phase, suggesting the presence of variable inter-star magnetospheric interaction. We also discover that the enhancement at periastron is confined to a very narrow orbital phase range ($\approx 5\%$ of the orbital period), but the X-ray properties close to periastron phase are similar to those observed away from periastron. From these observations, we infer that the underlying cause is magnetic reconnection heating the stellar wind plasma, rather than shocks produced by wind-wind collision. Finally, by comparing the behavior of $\epsilon$ Lupi with that observed for cooler magnetic binary systems, we propose that elevated X-ray flux at periastron phase is likely a general characteristic of interacting magnetospheres irrespective of the spectral types of the constituent stars., Comment: Accepted for publication in MNRAS (20 pages, 17 figures)
Published: 2023
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2. The long-term spectral changes of eta Carinae: are they caused by a dissipating occulter as indicated by CMFGEN models?

Author: Damineli, A., Hillier, D. J., Navarete, F., Moffat, A. F. J., Weigelt, G., Corcoran, M. F., Gull, T. R., Richardson, N. D., Ho, T. P., Madura, T. I., Espinoza-Galeas, D., Hartman, H., Morris, P., Pickett, C. S., Stevens, I. R., Russell, C. M. P., Hamaguchi, K., Jablonski, F. J., Teodoro, M., McGee, P., Cacella, P., Heathcote, B., Harrison, K., Johnston, M., Bohlsen, T., and Di Scala, G.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Eta Carinae ($\eta$\,Car) exhibits a unique set of P Cygni profiles with both broad and narrow components. Over many decades, the spectrum has changed -- there has been an increase in observed continuum fluxes and a decrease in FeII and HI emission line equivalent widths. The spectrum is evolving towards that of a P Cygni star such as P~Cygni itself and HDE~316285. The spectral evolution has been attributed to intrinsic variations such as a decrease in the mass-loss rate of the primary star or differential evolution in a latitudinal-dependent stellar wind. However intrinsic wind changes conflict with three observational results: the steady long-term bolometric luminosity; the repeating X-ray light curve over the binary period; and the constancy of the dust-scattered spectrum from the Homunculus. We extend previous work that showed a secular strengthening of P~Cygni absorptions by adding more orbital cycles to overcome temporary instabilities and by examining more atomic transitions. {\sc cmfgen} modeling of the primary wind shows that a time-decreasing mass-loss rate is not the best explanation for the observations. However, models with a `small' dissipating absorber in our line-of-site can explain both the increase in brightness and changes in the emission and P Cygni absorption profiles. If the spectral evolution is caused by the dissipating circumstellar medium, and not by intrinsic changes in the binary, the dynamical timescale to recover from the Great Eruption is much less than a century, different from previous suggestions., Comment: 71 pages, 8 figures, 4 long tables, to appear on ApJ
Published: 2022

3. Competitive X-ray and Optical Cooling in the Collisionless Shocks of WR 140

Author: Pollock, A. M. T., Corcoran, M. F., Stevens, I. R., Russell, C. M. P., Hamaguchi, K., Williams, P. M., Moffat, A. F. J., Weigelt, G., Shenavrin, V., Richardson, N. D., Espinoza, D., and Drake, S. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: WR 140 is a long-period, highly eccentric Wolf-Rayet star binary system with exceptionally well-determined orbital and stellar parameters. Bright, variable X-ray emission is generated in shocks produced by the collision of the winds of the WC7pd+O5.5fc component stars. We discuss the variations in the context of the colliding-wind model using broad-band spectrometry from the RXTE, SWIFT, and NICER observatories obtained over 20 years and nearly 1000 observations through 3 consecutive 7.94-year orbits including 3 periastron passages. The X-ray luminosity varies as expected with the inverse of the stellar separation over most of the orbit: departures near periastron are produced when cooling shifts to excess optical emission in CIII $\lambda5696$ in particular. We use X-ray absorption to estimate mass-loss rates for both stars and to constrain the system morphology. The absorption maximum coincides closely with inferior conjunction of the WC star and provides evidence of the ion-reflection mechanism that underlies the formation of collisionless shocks governed by magnetic fields probably generated by the Weibel instability. Comparisons with K-band emission and HeI $\lambda$10830 absorption show that both are correlated after periastron with the asymmetric X-ray absorption. Dust appears within a few days of periastron suggesting formation within shocked gas near the stagnation point. X-ray flares seen in $\eta$ Carinae have not occurred in WR 140, suggesting the absence of large-scale wind inhomogeneities. Relatively constant soft emission revealed during the X-ray minimum is probably not from recombining plasma entrained in outflowing shocked gas., Comment: 52 pages, 17+1 figures, Accepted for publication in The Astrophysical Journal 23 August 2021
Published: 2021
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4. An interview with Bernard Beckett

Author: Corcoran, M. Doyle
Published: 2012

5. How real is James Wood's real

Author: Corcoran, M. Doyle
Published: 2012

6. Spectroscopic Signatures of the Vanishing Natural Coronagraph of eta Carinae

Author: Damineli, A., Navarete, F., Hillier, D. J., Moffat, A. F. J., Corcoran, M. F., Gull, T. R., Richardson, N. D., Weigelt, G., Morris, P. W., and Stevens, I.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Eta Carinae is a massive interacting binary system shrouded in a complex circumstellar environment whose evolution is the source of the long-term brightening observed during the last 80 years. An occulter, acting as a natural coronagraph, impacts observations from our perspective, but not from most other directions. Other sight-lines are visible to us through studies of the Homunculus reflection nebula. The coronagraph appears to be vanishing, decreasing the extinction towards the central star, and causing the star's secular brightening. In contrast, the Homunculus remains at an almost constant brightness. The coronagraph primarily suppresses the stellar continuum, to a lesser extent the wind lines, and not the circumstellar emission lines. This explains why the absolute values of equivalent widths (EWs) of the emission lines in our direct view are larger than those seen in reflected by the Homunculus, why the direct view absolute EWs are decreasing with time, and why lower-excitation spectral wind lines formed at larger radii (e.g. FeII 4585A) decrease in intensity at a faster pace than higher excitation lines that form closer to the star (e.g. H\delta). Our main result is that the star, despite its 10-fold brightening over two decades, is relatively stable. A vanishing coronagraph that can explain both the large flux evolution and the much weaker spectral evolution. This is contrary to suggestions that the long-term variability is intrinsic to the primary star that is still recovering from the Great Eruption with a decreasing mass-loss rate and a polar wind that is evolving at a slower pace than at the equator., Comment: 20 pages, 10 figures, accepted on MNRAS (May 10th, 2021)
Published: 2021
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7. Comparison of $pp$ and $p \bar{p}$ differential elastic cross sections and observation of the exchange of a colorless $C$-odd gluonic compound

Author: Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Agnew, J. P., Alexeev, G. D., Alkhazov, G., Alton, A., Alves, G. A., Antchev, G., Askew, A., Aspell, P., Jesus, A. C. S. Assis, Atanassov, I., Atkins, S., Augsten, K., Aushev, V., Aushev, Y., Avati, V., Avila, C., Badaud, F., Baechler, J., Bagby, L., Barrera, C. Baldenegro, Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Barreto, J., Bartlett, J. F., Bassler, U., Bazterra, V., Bean, A., Begalli, M., Bellantoni, L., Berardi, V., Beri, S. B., Bernardi, G., Bernhard, R., Berretti, M., Bertram, I., Besanccon, M., Beuselinck, R., Bhat, P. C., Bhatia, S., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Boos, E. E., Borchsh, V., Borissov, G., Borysova, M., Bossini, E., Bottigli, U., Bozzo, M., Brandt, A., Brandt, O., Brochmann, M., Brock, R., Bross, A., Brown, D., Bu, X. B., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Burkhardt, H., Buszello, C. P., Cafagna, F. S., Camacho-P'erez, E., Carvahlo, W., Casey, B. C. K., Castilla-Valdez, H., Catanesi, M. G., Caughron, S., Chakrabarti, S., Chan, K. M., Chandra, A., Chapon, E., Chen, G., Cho, S. W., Choi, S., Choudhary, B., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Csan'ad, M., Cs"orgHo, T., Cuth, J., Cutts, D., Das, A., Davies, G., Deile, M., de Jong, S. J., De La Cruz-Burelo, E., De Leonardis, F., D'eliot, F., Demina, R., Denisov, D., Denisov, S. P., Desai, S., Deterre, C., DeVaughan, K., Diehl, H. T., Diesburg, M., Ding, P. F., Dominguez, A., Doubek, M., Drutskoy, A., Druzhkin, D., Dubey, A., Dudko, L. V., Duperrin, A., Dutt, S., Eads, M., Edmunds, D., Eggert, K., Ellison, J., Elvira, V. D., Enari, Y., Eremin, V., Evans, H., Evdokimov, A., Evdokimov, V. N., Faur'e, A., Feng, L., Ferbel, T., Ferro, F., Fiedler, F., Fiergolski, A., Filthaut, F., Fisher, W., Fisk, H. E., Forthomme, L., Fortner, M., Fox, H., Franc, J., Fuess, S., Garbincius, P. H., Garcia, F., Garcia-Bellido, A., Garc'ia-Gonz'alez, J. A., Gavrilov, V., Geng, W., Georgiev, V., Gerber, C. E., Gershtein, Y., Giani, S., Ginther, G., Gogota, O., Golovanov, G., Grannis, P. D., Greder, S., Greenlee, H., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Gr"unendahl, S., Gr"unewald, M. W., Grzanka, L., Guillemin, T., Gutierrez, G., Gutierrez, P., Haley, J., Hammerbauer, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hogan, J., Hohlfeld, M., Holzbauer, J. L., Howley, I., Hubacek, Z., Hynek, V., Iashvili, I., Ilchenko, Y., Illingworth, R., Isidori, T., Ito, A. S., Ivanchenko, V., Jabeen, S., Jaffr'e, M., Janda, M., Jayasinghe, A., Jeong, M. S., Jesik, R., Jiang, P., Johns, K., Johnson, E., Johnson, M., Jonckheere, A., Jonsson, P., Joshi, J., Jung, A. W., Juste, A., Kajfasz, E., Karev, A., Karmanov, D., Kavspar, J., Katsanos, I., Kaur, M., Kaynak, B., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Kiselevich, I., Kohli, J. M., Kopal, J., Kozelov, A. V., Kraus, J., Kumar, A., Kundr'at, V., Kupco, A., Kurvca, T., Kuzmin, V. A., Lami, S., Lammers, S., Latino, G., Lebrun, P., Lee, H. S., Lee, S. W., Lee, W. M., Le, X., Lellouch, J., Li, D., Li, H., Li, L., Li, Q. Z., Lim, J. K., Lincoln, D., Lindsey, C., Linhart, R., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, H., Liu, Y., Lobodenko, A., Lokajicek, M., Lokaj'ivcek, M. V., de Sa, R. Lopes, Losurdo, L., Rodr'iguez, F. Lucas, Luna-Garcia, R., Lyon, A. L., Maciel, A. K. A., Macr'i, M., Madar, R., na-Villalba, R. Maga, Malawski, M., Malbouisson, H. B., Malik, S., Malyshev, V. L., Mansour, J., Mart'inez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Miconi, F., Minafra, N., Minutoli, S., Molina, J., Mondal, N. K., Da Motta, H., Mulhearn, M., Mundim, L., Naaranoja, T., Nagy, E., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Nemes, F., Neustroev, P., Nguyen, H. T., Niewiadomski, H., Nov'ak, T., Nunnemann, T., Oguri, V., Oliveri, E., Oljemark, F., Orduna, J., Oriunno, M., Osman, N., "Osterberg, K., Pal, A., Palazzi, P., Parashar, N., Parihar, V., Park, S. K., Partridge, R., Parua, N., Pasechnik, R., Passaro, V., Patwa, A., Penning, B., Perfilov, M., Peroutka, Z., Peters, Y., Petridis, K., Petrillo, G., P'etroff, P., Pleier, M. -A., Podstavkov, V. M., Popov, A. V., Da Silva, W. L. Prado, Prewitt, M., Price, D., Proch'azka, J., Prokopenko, N., Qian, J., Quadt, A., Quinn, B., Quinto, M., Raben, T. G., Radermacher, E., Rangel, M., Radicioni, E., Ratoff, P. N., Ravotti, F., Razumov, I., Ripp-Baudot, I., Rizatdinova, F., Robutti, E., Rodrigues, R. F., Rominsky, M., Ross, A., Royon, C., Rubinov, P., Ruchti, R., Ruggiero, G., Saarikko, H., Sajot, G., Samoylenko, V. D., S'anchez-Hern'andez, A., Sanders, M. P., Santoro, A., Santos, A. S., Savage, G., Savitskyi, M., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schott, M., Schwanenberger, C., Schwienhorst, R., Scribano, A., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shaw, S., Shchukin, A. A., Shkola, O., Simak, V., Siroky, J., Skubic, P., Slattery, P., Smajek, J., Snoeys, W., Snow, G. R., Snow, J., Snyder, S., S"oldner-Rembold, S., Sonnenschein, L., Soustruznik, K., Stark, J., Stefaniuk, N., Stefanovitch, R., Ster, A., Stoyanova, D. A., Strauss, M., Suter, L., Svoisky, P., Szanyi, I., Sziklai, J., Taylor, C., Tcherniaev, E., Titov, M., Tokmenin, V. V., Tsai, Y. -T., Tsybychev, D., Tuchming, B., Tully, C., Turini, N., Urban, O., Uvarov, L., Uvarov, S., Uzunyan, S., Vacek, V., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Vavroch, O., Verkheev, A. Y., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vokac, P., Wahl, H. D., Wang, C., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weichert, J., Welti, J., Welty-Rieger, L., Williams, J., Williams, M. R. J., Wilson, G. W., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Yamada, R., Yang, S., Yasuda, T., Yatsunenko, Y. A., Ye, W., Ye, Z., Yin, H., Yip, K., Youn, S. W., Yu, J. M., Zennamo, J., Zhao, T. G., Zhou, B., Zhu, J., Zich, J., Zielinski, K., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We describe an analysis comparing the $p\bar{p}$ elastic cross section as measured by the D0 Collaboration at a center-of-mass energy of 1.96 TeV to that in $pp$ collisions as measured by the TOTEM Collaboration at 2.76, 7, 8, and 13 TeV using a model-independent approach. The TOTEM cross sections extrapolated to a center-of-mass energy of $\sqrt{s} =$ 1.96 TeV are compared with the D0 measurement in the region of the diffractive minimum and the second maximum of the $pp$ cross section. The two data sets disagree at the 3.4$\sigma$ level and thus provide evidence for the $t$-channel exchange of a colorless, $C$-odd gluonic compound, also known as the odderon. We combine these results with a TOTEM analysis of the same $C$-odd exchange based on the total cross section and the ratio of the real to imaginary parts of the forward elastic scattering amplitude in $pp$ scattering. The combined significance of these results is larger than 5$\sigma$ and is interpreted as the first observation of the exchange of a colorless, $C$-odd gluonic compound., Comment: D0 and TOTEM Collaborations
Published: 2020
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8. On the changes in the physical properties of the ionized region around the Weigelt structures in Eta Carinae over the 5.54-yr spectroscopic cycle

Author: Teodoro, M., Gull, T. R., Bautista, M. A., Hillier, D. J., Weigelt, G, and Corcoran, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present HST/STIS observations and analysis of two prominent nebular structures around the central source of Eta Carinae, the knots C and D. The former is brighter than the latter for emission lines from intermediate or high ionization potential ions. The brightness of lines from intermediate and high ionization potential ions significantly decreases at phases around periastron. We do not see conspicuous changes in the brightness of lines from low ionization potential (<13.6 eV) that the total extinction towards the Weigelt structures is that the total extinction towards the Weigelt structures is AsubV =2/0. that the total extinction towards the Weigelt structures is AV = 2.0. Weigelt C and D are characterized by an electron density of that the total extinction towards the Weigelt structures is AV = 2.0. Weigelt C and D are characterized by an electron density of 10exp6.9 cm-3 that does not significantly change throughout the orbital cycle. The electron temperature varies from 5500 K (around periastron) to 7200 K (around apastron). The relative changes in the brightness of He I lines are well reproduced by the variations in the electron temperature alone. We found that, at phases around periastron, the electron temperature seems to be higher for Weigelt C than that of D. The Weigelt structures are located close to the Homunculus equatorial plane, at a distance of about 1240 AU from the central source. From the analysis of proper motion and age, the Weigelt complex can be associated with the equatorial structure called the Butterfly Nebula surrounding the central binary system., Comment: 19 pages, 18 figures
Published: 2020
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9. The high-energy emission from HD~93129A near periastron

Author: del Palacio, S., García, F., Altamirano, D., Barbá, R. H., Bosch-Ramon, V., Corcoran, M., De Becker, M., Hamaguchi, K., Apellániz, J. Maíz, Adrover, P. Munar, Paredes, J. M., Romero, G. E., Sana, H., Tavani, M., and ud-Doula, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD~93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites \textit{Chandra} and \textit{NuSTAR} and the $\gamma$-ray satellite \textit{AGILE}. High-energy emission coincident with HD~93129A was detected in the X-ray band up to $\sim$18~keV, whereas in the $\gamma$-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, $f_\mathrm{NT,e} < 0.02$. In addition, we set a lower limit for the magnetic field in the wind-collision region as $B_\mathrm{WCR} > 0.3$~G. We also argue a putative interpretation of the emission from which we estimate $f_\mathrm{NT,e} \approx 0.006$ and $B_\mathrm{WCR} \approx 0.5$~G. We conclude that multi-wavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterising the relativistic particle content and magnetic field intensity in colliding wind binaries., Comment: 11 pages, 10 figures, accepted for publication in MNRAS
Published: 2020
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10. Early detection of subclinical mastitis in lactating dairy cows using cow-level features

Author: Pakrashi, A., Ryan, C., Guéret, C., Berry, D.P., Corcoran, M., Keane, M.T., and Mac Namee, B.
Published: 2023
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11. A Measurement of the Branching Ratio of $\pi^0$ Dalitz Decay using $K_L \rightarrow \pi^0\pi^0\pi^0$ Decays

Author: Abouzaid, E., Arenton, M., Barker, A. R., Bellantoni, L., Blucher, E., Bock, G. J., Cheu, E., Coleman, R., Corcoran, M. D., Cox, B., Erwin, A. R., Escobar, C. O., Glazov, A., Golossanov, A., Gomes, R. A., Gouffon, P., Hsiung, Y. B., Jensen, D. A., Kessler, R., Kotera, K., Ledovskoy, A., McBride, P. L., Monnier, E., Nguyen, H., Niclasen, R., Phillips II, D. G., Ramberg, E. J., Ray, R. E., Ronquest, M., Santos, E., Slater, W., Smith, D., Solomey, N., Swallow, E. C., Toale, P. A., Tschirhart, R., Wah, Y. W., Wang, J., White, H. B., Whitmore, J., Wilking, M. J., Winstein, B., Winston, R., Worcester, E. T., Yamanaka, T., Zimmerman, E. D., and Zukanovich, R. F.
Subjects: High Energy Physics - Experiment
Abstract: We present a measurement of $B(\pi^0 \rightarrow e^+e^- \gamma)/B(\pi^0 \rightarrow \gamma\gamma)$, the Dalitz branching ratio, using data taken in 1999 by the E832 KTeV experiment at Fermi National Accelerator Laboratory. We use neutral pions from fully reconstructed $K_L$ decays in flight; the measurement is based on about 60 thousand $K_L \rightarrow \pi^0\pi^0\pi^0 \rightarrow \gamma\gamma~\gamma\gamma~e^+e^-\gamma$ decays. We normalize to $K_L \rightarrow \pi^0\pi^0\pi^0 \rightarrow 6\gamma$ decays. We find $B(\pi^0 \rightarrow e^+e^- \gamma)/B(\pi^0 \rightarrow \gamma\gamma)$ $(m_{e^+e^-}$ > 15 MeV/$c^2)$ = $[3.920 \pm 0.016(stat) \pm 0.036 (syst)] \times 10^{-3}$. Using the Mikaelian and Smith prediction for the $e^+e^-$ mass spectrum, we correct the result to the full $e^+e^-$ mass range. The corrected result is $B(\pi^0 \rightarrow e^+e^- \gamma)/B(\pi^0 \rightarrow \gamma\gamma) = [1.1559 \pm 0.0047(stat) \pm 0.0106 (syst)]$%. This result is consistent with previous measurements and the uncertainty is a factor of three smaller than any previous measurement., Comment: 11 pages, 7 figures; v2 accepted version
Published: 2019
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12. VLTI-AMBER velocity-resolved aperture-synthesis imaging of Eta Carinae with a spectral resolution of 12000. Studies of the primary star wind and innermost wind-wind collision

Author: Weigelt, G., Hofmann, K. -H., Schertl, D., Clementel, N., Corcoran, M. F., Damineli, A., de Wit, W. -J., Grellmann, R., Groh, J., Guieu, S., Gull, T., Heininger, M., Hillier, D. J., Hummel, C. A., Kraus, S., Madura, T., Mehner, A., Mérand, A., Millour, F., Moffat, A. F. J., Ohnaka, K., Patru, F., Petrov, R. G., Rengaswamy, S., Richardson, N. D., Rivinius, T., Schöller, M., Teodoro, M., and Wittkowski, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Context. The mass loss from massive stars is not understood well. Eta Car is a unique object for studying the massive stellar wind during the LBV phase. It is also an eccentric binary with a period of 5.54 yr. The nature of both stars is uncertain, although we know from X-ray studies that there is a wind-wind collision whose properties change with orbital phase. Methods. Observations of Eta Car were carried out with the ESO VLTI and the AMBER instrument between approximately five and seven months before the August 2014 periastron passage. Velocity-resolved aperture-synthesis images were reconstructed from the spectrally dispersed interferograms. Interferometric studies can provide information on the binary orbit, the primary wind, and the wind collision. Results. We present velocity-resolved aperture-synthesis images reconstructed in more than 100 different spectral channels distributed across the Br Gamma 2.166 micrometer emission line. The intensity distribution of the images strongly depends on wavelength. At wavelengths corresponding to radial velocities of approximately -140 to -376 km/s measured relative to line center, the intensity distribution has a fan-shaped structure. At the velocity of -277 km/s, the position angle of the symmetry axis of the fan is ~ 126 degree. The fan-shaped structure extends approximately 8.0 mas (~ 18.8 au) to the southeast and 5.8 mas (~ 13.6 au) to the northwest, measured along the symmetry axis at the 16% intensity contour. The shape of the intensity distributions suggests that the obtained images are the first direct images of the innermost wind-wind collision zone. Therefore, the observations provide velocity-dependent image structures that can be used to test three-dimensional hydrodynamical, radiative transfer models of the massive interacting winds of Eta Car.
Published: 2016
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13. He II $\lambda$4686 emission from the massive binary system in $\eta$ Car: constraints to the orbital elements and the nature of the periodic minima

Author: Teodoro, M., Damineli, A., Heathcote, B., Richardson, N. D., Moffat, A. F. J., St-Jean, L., Russell, C., Gull, T. R., Madura, T. I., Pollard, K. R., Walter, F., Coimbra, A., Prates, R., Fernández-Lajús, E., Gamen, R. C., Hickel, G., Henrique, W., Navarete, F., Andrade, T., Jablonski, F., Luckas, P., Locke, M., Powles, J., Bohlsen, T., Chini, R., Corcoran, M. F., Hamaguchi, K., Groh, J. H., Hillier, D. J., and Weigelt, G.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: {\eta} Carinae is an extremely massive binary system in which rapid spectrum variations occur near periastron. Most notably, near periastron the He II $\lambda 4686$ line increases rapidly in strength, drops to a minimum value, then increases briefly before fading away. To understand this behavior, we conducted an intense spectroscopic monitoring of the He II $\lambda 4686$ emission line across the 2014.6 periastron passage using ground- and space-based telescopes. Comparison with previous data confirmed the overall repeatability of EW(He II $\lambda 4686$), the line radial velocities, and the timing of the minimum, though the strongest peak was systematically larger in 2014 than in 2009 by 26%. The EW(He II $\lambda 4686$) variations, combined with other measurements, yield an orbital period $2022.7\pm0.3$ d. The observed variability of the EW(He II $\lambda 4686$) was reproduced by a model in which the line flux primarily arises at the apex of the wind-wind collision and scales inversely with the square of the stellar separation, if we account for the excess emission as the companion star plunges into the hot inner layers of the primary's atmosphere, and including absorption from the disturbed primary wind between the source and the observer. This model constrains the orbital inclination to $135^\circ$-$153^\circ$, and the longitude of periastron to $234^\circ$-$252^\circ$. It also suggests that periastron passage occurred on $T_0 = 2456874.4\pm1.3$ d. Our model also reproduced EW(He II $\lambda 4686$) variations from a polar view of the primary star as determined from the observed He II $\lambda 4686$ emission scattered off the Homunculus nebula., Comment: The article contains 23 pages and 17 figures. It has been accepted for publication in ApJ
Published: 2016
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14. The X-ray Lightcurve of the Supermassive star eta Carinae, 1996--2014

Author: Corcoran, M. F., Hamaguchi, K., Liburd, J. K., Morris, D., Gull, T. R., Madura, T. I., Teodoro, M., Moffat, A. F. J., Richardson, N. D., Russell, C. M. P., Pollock, A. M. T., and Owocki, S. P.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Eta Carinae is the nearest example of a supermassive, superluminous, unstable star. Mass loss from the system is critical in shaping its circumstellar medium and in determining its ultimate fate. Eta Car currently loses mass via a dense, slow stellar wind and possesses one of the largest mass loss rates known. It is prone to episodes of extreme mass ejection via eruptions from some as-yet unspecified cause; the best examples of this are the large-scale eruptions which occurred in 19th century. Eta Car is a colliding wind binary in which strong variations in X-ray emission and in other wavebands are driven by the violent collision of the wind of eta Car-A and the fast, less dense wind of an otherwise hidden companion star. X-ray variations are the simplest diagnostic we have to study the wind-wind collision and allow us to measure the state of the stellar mass loss from both stars. We present the X-ray lightcurve over the last 20 years from ROSAT observations and monitoring with the Rossi X-ray Timing Explorer and the X-ray Telescope on the Swift satellite. We compare and contrast the behavior of the X-ray emission from the system over that timespan, including surprising variations during the 2014 X-ray minimum., Comment: International Workshop on Wolf-Rayet Stars, Potsdam, Germany, 1 - 5 June 2015
Published: 2015

15. A Coordinated X-ray and Optical Campaign on the Nearest Massive Eclipsing Binary, Delta Ori Aa: I. Overview of the X-ray Spectrum

Author: Corcoran, M. F., Nichols, J. S., Pablo, H., Shenar, T., Pollock, A. M. T., Waldron, W. L., Moffat, A. F. J., Richardson, N. D., Russell, C. M. P., Hamaguchi, K., Huenemoerder, D. P., Oskinova, L., Hamann, W. -R., Naze, Y., Ignace, R., Evans, N. R., Lomax, J. R., Hoffman, J. L., Gayley, K., Owocki, S. P., Leutenegger, M., Gull, T. R., Hole, K. T., Lauer, J., and Iping, R. C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present an overview of four phase-constrained Chandra HETGS X-ray observations of Delta Ori A. Delta Ori A is actually a triple system which includes the nearest massive eclipsing spectroscopic binary, Delta Ori Aa, the only such object which can be observed with little phase-smearing with the Chandra gratings. Since the fainter star, Delta Ori Aa2, has a much lower X-ray luminosity than the brighter primary, Delta Ori A provides a unique system with which to test the spatial distribution of the X-ray emitting gas around Delta Ori Aa1 via occultation by the photosphere of and wind cavity around the X-ray dark secondary. Here we discuss the X-ray spectrum and X-ray line profiles for the combined observation, having an exposure time of nearly 500 ksec and covering nearly the entire binary orbit. Companion papers discuss the X-ray variability seen in the Chandra spectra, present new space-based photometry and ground-based radial velocities simultaneous with the X-ray data to better constrain the system parameters, and model the effects of X-rays on the optical and UV spectrum. We find that the X-ray emission is dominated by embedded wind shock emission from star Aa1, with little contribution from the tertiary star Ab or the shocked gas produced by the collision of the wind of Aa1 against the surface of Aa2. We find a similar temperature distribution to previous X-ray spectrum analyses. We also show that the line half-widths are about $0.3-0.5\times$ the terminal velocity of the wind of star Aa1. We find a strong anti-correlation between line widths and the line excitation energy, which suggests that longer-wavelength, lower-temperature lines form farther out in the wind. Our analysis also indicates that the ratio of the intensities of the strong and weak lines of \ion{Fe}{17} and \ion{Ne}{10} are inconsistent with model predictions, which may be an effect of resonance scattering, Comment: accepted by ApJ; revised according to ApJ proof
Published: 2015
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16. A Coordinated X-ray and Optical Campaign of the Nearby Massive Binary $\delta$ Orionis Aa: II. X-ray Variability

Author: Nichols, J. S., Huenemoerder, D. P., Corcoran, M. F., Waldron, W., Nazé, Y., Pollock, A. M. T., Moffat, A. F. J., Lauer, J., Shenar, T., Russell, C. M. P., Richardson, N. D., Pablo, H., Evans, N R., Hamaguchi, K., Gull, T., Hamann, W. R., Oskinova, L., Ignace, R., Hoffman, Jennifer L., Hole, K. T., and Lomax, J. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present time-resolved and phase-resolved variability studies of an extensive X-ray high-resolution spectral dataset of the $\delta$ Orionis Aa binary system. The four observations, obtained with Chandra ACIS HETGS, have a total exposure time of ~479 ks and provide nearly complete binary phase coverage. Variability of the total X-ray flux in the range 5-25 $\AA$ is confirmed, with maximum amplitude of about +/-15% within a single ~125 ks observation. Periods of 4.76d and 2.04d are found in the total X-ray flux, as well as an apparent overall increase in flux level throughout the 9-day observational campaign. Using 40 ks contiguous spectra derived from the original observations, we investigate variability of emission line parameters and ratios. Several emission lines are shown to be variable, including S XV, Si XIII, and Ne IX. For the first time, variations of the X-ray emission line widths as a function of the binary phase are found in a binary system, with the smallest widths at phase=0.0 when the secondary $\delta$ Orionis Aa2 is at inferior conjunction. Using 3D hydrodynamic modeling of the interacting winds, we relate the emission line width variability to the presence of a wind cavity created by a wind-wind collision, which is effectively void of embedded wind shocks and is carved out of the X-ray-producing primary wind, thus producing phase-locked X-ray variability., Comment: 36 pages, 14 Tables, 19 Figures, accepted by ApJ, one of 4 related papers to be published together
Published: 2015
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17. A coordinated X-ray and Optical Campaign of the Nearest Massive Eclipsing Binary, $\delta$ Orionis Aa: IV. A multiwavelength, non-LTE spectroscopic analysis

Author: Shenar, T., Oskinova, L., Hamann, W. -R., Corcoran, M. F., Moffat, A. F. J., Pablo, H., Richardson, N. D., Waldron, W. L., Huenemoerder, D. P., Apellániz, J. Maíz, Nichols, J. S., Todt, H., Nazé, Y., Hoffman, J. L., Pollock, A. M. T., and Negueruela, I.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Eclipsing systems of massive stars allow one to explore the properties of their components in great detail. We perform a multi-wavelength, non-LTE analysis of the three components of the massive multiple system $\delta$ Ori A, focusing on the fundamental stellar properties, stellar winds, and X-ray characteristics of the system. The primary's distance-independent parameters turn out to be characteristic for its spectral type (O9.5 II), but usage of the ${\rm \it Hipparcos}$ parallax yields surprisingly low values for the mass, radius, and luminosity. Consistent values follow only if $\delta$ Ori lies at about twice the ${\rm \it Hipparcos}$ distance, in the vicinity of the $\sigma$-Orionis cluster. The primary and tertiary dominate the spectrum and leave the secondary only marginally detectable. We estimate the V-band magnitude difference between primary and secondary to be $\Delta V \approx 2.\!\!^{\rm m}8$. The inferred parameters suggest the secondary is an early B-type dwarf ($\approx$ B1 V), while the tertiary is an early B-type subgiant ($\approx$ B0 IV). We find evidence for rapid turbulent velocities ($\sim 200$ km ${\rm s}^{-1}$) and wind inhomogeneities, partially optically thick, in the primary's wind. The bulk of the X-ray emission likely emerges from the primary's stellar wind ($\log L_{\text{X}} / L_{\text{Bol}} \approx -6.85$), initiating close to the stellar surface at $R_0 \sim 1.1\,R_*$. Accounting for clumping, the mass-loss rate of the primary is found to be $\log \dot{M} \approx -6.4\,[M_\odot\,{\rm yr}^{-1}]$, which agrees with hydrodynamic predictions, and provides a consistent picture along the X-ray, UV, optical and radio spectral domains., Comment: Accepted for Publication in APJ, 21 pages, 16 figures and 2 tables
Published: 2015
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18. Mu2e Technical Design Report

Author: Bartoszek, L., Barnes, E., Miller, J. P., Mott, J., Palladino, A., Quirk, J., Roberts, B. L., Crnkovic, J., Polychronakos, V., Tishchenko, V., Yamin, P., Cheng, C. -h., Echenard, B., Flood, K., Hitlin, D. G., Kim, J. H., Miyashita, T. S., Porter, F. C., Röhrken, M., Trevor, J., Zhu, R. -Y., Heckmaier, E., Kang, T. I., Lim, G., Molzon, W., You, Z., Artikov, A. M., Budagov, J. A., Davydov, Yu. I., Glagolev, V. V., Simonenko, A. V., Usubov, Z. U., Oh, S. H., Wang, C., Ambrosio, G., Andreev, N., Arnold, D., Ball, M., Bernstein, R. H., Bianchi, A., Biery, K., Bossert, R., Bowden, M., Brandt, J., Brown, G., Brown, H., Buehler, M., Campbell, M., Cheban, S., Chen, M., Coghill, J., Coleman, R., Crowley, C., Deshpande, A., Deuerling, G., Dey, J., Dhanaraj, N., Dinnon, M., Dixon, S., Drendel, B., Eddy, N., Evans, R., Evbota, D., Fagan, J., Feher, S., Fellenz, B., Friedsam, H., Gallo, G., Gaponenko, A., Gardner, M., Gaugel, S., Genser, K., Ginther, G., Glass, H., Glenzinski, D., Hahn, D., Hansen, S., Hartsell, B., Hays, S., Hocker, J. A., Huedem, E., Huffman, D., Ibrahim, A., Johnstone, C., Kashikhin, V., Kashikhin, V. V., Kasper, P., Kiper, T., Knapp, D., Knoepfel, K., Kokoska, L., Kozlovsky, M., Krafczyk, G., Kramp, M., Krave, S., Krempetz, K., Kutschke, R. K., Kwarciany, R., Lackowski, T., Lamm, M. J., Larwill, M., Leavell, F., Leeb, D., Leveling, A., Lincoln, D., Logashenko, V., Lombardo, V., Lopes, M. L., Makulski, A., Martinez, A., McArthur, D., McConologue, F., Michelotti, L., Mokhov, N., Morgan, J., Mukherjee, A., Murat, P., Nagaslaev, V., Neuffer, D. V., Nicol, T., Niehoff, J., Nogiec, J., Olson, M., Orris, D., Ostojic, R., Page, T., Park, C., Peterson, T., Pilipenko, R., Pla-Dalmau, A., Poloubotko, V., Popovic, M., Prebys, E., Prieto, P., Pronskikh, V., Pushka, D., Rabehl, R., Ray, R. E., Rechenmacher, R., Rivera, R., Robotham, W., Rubinov, P., Rusu, V. L., Scarpine, V., Schappert, W., Schoo, D., Stefanik, A., Still, D., Tang, Z., Tanovic, N., Tartaglia, M., Tassotto, G., Tinsley, D., Tschirhart, R. S., Vogel, G., Wagner, R., Wands, R., Wang, M., Werkema, S., White Jr., H. B., Whitmore, J., Wielgos, R., Woods, R., Worel, C., Zifko, R., Ciambrone, P., Colao, F., Cordelli, M., Corradi, G., Dane, E., Giovannella, S., Happacher, F., Luca, A., Miscetti, S., Ponzio, B., Pileggi, G., Saputi, A., Sarra, I., Soleti, R. S., Stomaci, V., Martini, M., Fabbricatore, P., Farinon, S., Musenich, R., Alexander, D., Daniel, A., Empl, A., Hungerford, E. V., Lau, K., Gollin, G. D., Huang, C., Roderick, D., Trundy, B., Brown, D. Na., Ding, D., Kolomensky, Yu. G., Lee, M. J., Cascella, M., Grancagnolo, F., Ignatov, F., Innocente, A., L'Erario, A., Miccoli, A., Maffezzoli, A., Mazzotta, P., Onorato, G., Piacentino, G. M., Rella, S., Rossetti, F., Spedicato, M., Tassielli, G., Taurino, A., Zavarise, G., Hooper, R., Brown, D. No., Djilkibaev, R., Matushko, V., Ankenbrandt, C., Boi, S., Dychkant, A., Hedin, D., Hodge, Z., Khalatian, V., Majewski, R., Martin, L., Okafor, U., Pohlman, N., Riddel, R. S., Shellito, A., de Gouvea, A. L., Cervelli, F., Carosi, R., Di Falco, S., Donati, S., Lomtadze, T., Pezzullo, G., Ristori, L., Spinella, F., Jones, M., Corcoran, M. D., Orduna, J., Rivera, D., Bennett, R., Caretta, O., Davenne, T., Densham, C., Loveridge, P., Odell, J., Bomgardner, R., Dukes, E. C., Ehrlich, R., Frank, M., Goadhouse, S., Group, R., Ho, E., Ma, H., Oksuzian, Y., Purvis, J., Wu, Y., Hertzog, D. W., Kammel, P., Lynch, K. R., and Popp, J. L.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The Mu2e experiment at Fermilab will search for charged lepton flavor violation via the coherent conversion process mu- N --> e- N with a sensitivity approximately four orders of magnitude better than the current world's best limits for this process. The experiment's sensitivity offers discovery potential over a wide array of new physics models and probes mass scales well beyond the reach of the LHC. We describe herein the preliminary design of the proposed Mu2e experiment. This document was created in partial fulfillment of the requirements necessary to obtain DOE CD-2 approval., Comment: compressed file, 888 pages, 621 figures, 126 tables; full resolution available at http://mu2e.fnal.gov; corrected typo in background summary, Table 3.4
Published: 2015

19. The Impact of Childhood Trauma on Developing Bipolar Disorder: Current Understanding and Ensuring Continued Progress

Author: Quidé Y, Tozzi L, Corcoran M, Cannon DM, and Dauvermann MR
Subjects: bipolar disorder, childhood trauma, vulnerability, early onset, peripheral blood marker, brain, Neurosciences. Biological psychiatry. Neuropsychiatry, RC321-571, Neurology. Diseases of the nervous system, RC346-429
Abstract: Yann Quidé,1,2 Leonardo Tozzi,3 Mark Corcoran,4 Dara M Cannon,5 Maria R Dauvermann6,7 1School of Psychiatry, University of New South Wales (UNSW), Sydney, NSW, Australia; 2Neuroscience Research Australia, Randwick, NSW, Australia; 3Department of Psychiatry and Behavioral Sciences, Stanford University, Stanford, CA, USA; 4School of Psychology, National University of Ireland Galway, Galway, Ireland; 5Centre for Neuroimaging & Cognitive Genomics (NICOG), Clinical Neuroimaging Laboratory, NCBES Galway Neuroscience Centre, School of Medicine, National University of Ireland Galway, Galway, Ireland; 6Department of Psychiatry, University of Cambridge, Cambridge, UK; 7McGovern Institute for Brain Research, Massachusetts Institute of Technology, Cambridge, MA, USACorrespondence: Maria R DauvermannDepartment of Psychiatry, University of Cambridge, Clifford Allbutt Building, Cambridge Biomedical Campus Box 58, Cambridge CB2 0XY, UKTel +441223 465246Email md874@medschl.cam.ac.ukAbstract: Childhood trauma (CT) has been repeatedly linked to earlier onset and greater severity of bipolar disorder (BD) in adulthood. However, such knowledge is mostly based on retrospective and cross-sectional studies in adults with BD. The first objective of this selective review is to characterize the short-term effects of CT in the development of BD by focusing on studies in young people. The second objective is to describe the longer-term consequences of CT by considering studies with adult participants. This review first outlines the most prominent hypotheses linking CT exposure and the onset of BD. Then, it summarizes the psychological and biological risk factors implicated in the development of BD, followed by a discussion of original studies that investigated the role of CT in young people with early-onset BD, youths at increased risk of developing BD, or young people with BD with a focus on subclinical and clinical outcome measures. The review considers additional biological and psychological factors associated with a negative impact of CT on the long-term course of BD in later adulthood. Finally, we discuss how the integration of information of CT can improve ongoing early identification of BD and mitigate severe clinical expression in later adulthood.Keywords: bipolar disorder, childhood trauma, vulnerability, early onset, peripheral blood marker, brain
Published: 2020

20. Integration of Artificial Intelligence into Metallography: Area-wide Analysis of Microstructural Components of a Jominy Sample

Author: Schneider, J., primary, Rostami, R., additional, Corcoran, M., additional, and Korpala, G., additional
Published: 2024
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21. Discrete absorption components in the massive LBV Binary MWC 314

Author: Lobel, A., Martayan, C., Corcoran, M., Groh, J. H., and Frémat, Y.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We investigate the physical properties of large-scale wind structures around massive hot stars with radiatively-driven winds. We observe Discrete Absorption Components (DACs) in optical He I P Cygni lines of the LBV binary MWC 314 (Porb=60.8 d). The DACs are observed during orbital phases when the primary is in front of the secondary star. They appear at wind velocities between -100 km/s and -600 km/s in the P Cyg profiles of He I lam5875, lam6678, and lam4471, signaling high-temperature expanding wind regions of enhanced density and variable outflow velocity. The DACs can result from wave propagation linked to the orbital motion near the low-velocity wind base. The He I lines indicate DAC formation close to the primary's surface in high-temperature wind regions in front of its orbit, or in dynamical wind regions confined between the binary stars. We observed the DACs with Mercator-HERMES on 5 Sep 2009, 5 May 2012, and 6 May 2014 when the primary is in front of the secondary star. XMM-Newton observations of 6 May 2014 significantly detected MWC 314 in X-rays at an average rate of ~0.015 cts/s., Comment: 2 pages, 2 figures, to appear in IAUS 307, 2014, Proc. of New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry, Geneva, Switzerland, June 23-27, 2014
Published: 2014
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22. The three-dimensional structure of the Eta Carinae Homunculus

Author: Steffen, W., Teodoro, M., Madura, T. I., Groh, J. H., Gull, T. R., Mehner, A., Corcoran, M. F., Damineli, A., and Hamaguchi, K.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We investigate, using the modeling code SHAPE, the three-dimensional structure of the bipolar Homunculus nebula surrounding Eta Carinae, as mapped by new ESO VLT/X-Shooter observations of the H2 $\lambda=2.12125$ micron emission line. Our results reveal for the first time important deviations from the axisymmetric bipolar morphology: 1) circumpolar trenches in each lobe positioned point-symmetrically from the center and 2) off-planar protrusions in the equatorial region from each lobe at longitudinal (~55 degrees) and latitudinal (10-20 degrees) distances from the projected apastron direction of the binary orbit. The angular distance between the protrusions (~110 degrees) is similar to the angular extent of each polar trench (~130 degrees) and nearly equal to the opening angle of the wind-wind collision cavity (~110 degrees). As in previous studies, we confirm a hole near the centre of each polar lobe and no detectable near-IR H2 emission from the thin optical skirt seen prominently in visible imagery. We conclude that the interaction between the outflows and/or radiation from the central binary stars and their orientation in space has had, and possibly still has, a strong influence on the Homunculus. This implies that prevailing theoretical models of the Homunculus are incomplete as most assume a single star origin that produces an axisymmetric nebula. We discuss how the newly found features might be related to the Homunculus ejection, the central binary and the interacting stellar winds. We also include a 3D printable version of our Homunculus model., Comment: 14 pages, 7 color figures, 1 interactive 3D figure (Figure 5, requires Adobe Reader), published in MNRAS. A 3D printable version of our Homunculus model can be downloaded from http://svs.gsfc.nasa.gov/vis/a010000/a011500/a011568/Eta_Car_Homunuculus_3D_model.zip or from the 'Supporting Information' link in the electronic version of the MNRAS article
Published: 2014
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23. Combination of CDF and D0 W-Boson Mass Measurements

Author: CDF Collaboration, Aaltonen, T., Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Bae, T., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Bromberg, C., Brucken, E., Budagov, J., Budd, H. S., Burkett, K., Busetto, G., Bussey, P., Butti, P., Buzatu, A., Calamba, A., Camarda, S., Campanelli, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Cho, K., Chokheli, D., Clark, A., Clarke, C., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Cremonesi, M., Cruz, D., Cuevas, J., Culbertson, R., d'Ascenzo, N., Datta, M., de Barbaro, P., Demortier, L., Marchese, L., Deninno, M., Devoto, F., D'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dorigo, M., Driutti, A., Ebina, K., Edgar, R., Elagin, A., Erbacher, R., Errede, S., Esham, B., Eusebi, R., Farrington, S., Ramos, J. P. Fernández, Field, R., Flanagan, G., Forrest, R., Franklin, M., Freeman, J. C., Frisch, H., Funakoshi, Y., Galloni, C., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., López, O. González, Gorelov, I., Goshaw, A. T., Goulianos, K., Gramellini, E., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Hahn, S. R., Han, J. Y., Happacher, F., Hara, K., Hare, M., Harr, R. F., Harrington-Taber, T., Hatakeyama, K., Hays, C., Heinrich, J., Herndon, M., Hocker, A., Hong, Z., Hopkins, W., Hou, S., Hughes, R. E., Husemann, U., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jindariani, S., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kambeitz, M., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Kilminster, B., Kim, D. H., Kim, H. S., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kim, Y. J., Kimura, N., Kirby, M., Knoepfel, K., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Kruse, M., Kuhr, T., Kurata, M., Laasanen, A. T., Lammel, S., Lancaster, M., Lannon, K., Latino, G., Lee, H. S., Lee, J. S., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lipeles, E., Lister, A., Liu, H., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucà, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maestro, P., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, P., Martínez, M., Matera, K., Mattson, M. E., Mazzacane, A., Mazzanti, P., McNulty, R., Mehta, A., Mehtala, P., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Moon, C. S., Moore, R., Morello, M. J., Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Nigmanov, T., Nodulman, L., Noh, S. Y., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Pagliarone, C., Palencia, E., Palni, P., Papadimitriou, V., Parker, W., Pauletta, G., Paulini, M., Paus, C., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Prokoshin, F., Pranko, A., Ptohos, F., Punzi, G., Ranjan, N., Fernández, I. Redondo, Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodriguez, T., Rolli, S., Ronzani, M., Roser, R., Rosner, J. L., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Sakumoto, W. K., Sakurai, Y., Santi, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, E. E., Schwarz, T., Scodellaro, L., Scuri, F., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Shalhout, S. Z., Shears, T., Shekhar, R., Shepard, P. F., Shimojima, M., Shochet, M., Shreyber-Tecker, I., Simonenko, A., Sliwa, K., Smith, J. R., Snider, F. D., Sorin, V., Song, H., Stancari, M., Denis, R. St., Stentz, D., Strologas, J., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thompson, D. S., Thomson, E., Thukral, V., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Ukegawa, F., Uozumi, S., Vázquez, F., Velev, G., Vellidis, C., Vernieri, C., Vidal, M., Vilar, R., Vizán, J., Vogel, M., Volpi, G., Wagner, P., Wallny, R., Wang, S. M., Waters, D., Wester III, W. C., Whiteson, D., Wicklund, A. B., Wilbur, S., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamato, D., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Zanetti, A. M., Zeng, Y., Zhou, C., Zucchelli, S., Collaboration, D0, Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Agnew, J. P., Alexeev, G. D., Alkhazov, G., Alton, A., Askew, A., Atkins, S., Augsten, K., Avila, C., Badaud, F., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Bartlett, J. F., Bassler, U., Bazterra, V., Bean, A., Begalli, M., Bellantoni, L., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besançon, M., Beuselinck, R., Bhat, P. C., Bhatia, S., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Boos, E. E., Borissov, G., Brandt, A., Brandt, O., Brock, R., Bross, A., Brown, D., Bu, X. B., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Buszello, C. P., Camacho-Pérez, E., Casey, B. C. K., Castilla-Valdez, H., Caughron, S., Chakrabarti, S., Chan, K. M., Chandra, A., Chapon, E., Chen, G., Cho, S. W., Choi, S., Choudhary, B., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Cutts, D., Das, A., Davies, G., de Jong, S. J., De La Cruz-Burelo, E., Déliot, F., Demina, R., Denisov, D., Denisov, S. P., Desai, S., Deterre, C., DeVaughan, K., Diehl, H. T., Diesburg, M., Ding, P. F., Dominguez, A., Dubey, A., Dudko, L. V., Duperrin, A., Dutt, S., Eads, M., Edmunds, D., Ellison, J., Elvira, V. D., Enari, Y., Evans, H., Evdokimov, V. N., Feng, L., Ferbel, T., Fiedler, F., Filthaut, F., Fisher, W., Fisk, H. E., Fortner, M., Fox, H., Fuess, S., Garcia-Bellido, A., García-González, J. A., Gavrilov, V., Geng, W., Gerber, C. E., Gershtein, Y., Ginther, G., Golovanov, G., Grannis, P. D., Greder, S., Greenlee, H., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grünendahl, S., Grünewald, M. W., Guillemin, T., Gutierrez, G., Gutierrez, P., Haley, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hogan, J., Hohlfeld, M., Holzbauer, J. L., Howley, I., Hubacek, Z., Hynek, V., Iashvili, I., Ilchenko, Y., Illingworth, R., Ito, A. S., Jabeen, S., Jaffré, M., Jayasinghe, A., Jeong, M. S., Jesik, R., Jiang, P., Johns, K., Johnson, E., Johnson, M., Jonckheere, A., Jonsson, P., Joshi, J., Jung, A. W., Juste, A., Kajfasz, E., Karmanov, D., Katsanos, I., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Kiselevich, I., Kohli, J. M., Kozelov, A. V., Kraus, J., Kumar, A., Kupco, A., Kurča, T., Kuzmin, V. A., Lammers, S., Lebrun, P., Lee, S. W., Lee, W. M., Lei, X., Lellouch, J., Li, D., Li, H., Li, L., Li, Q. Z., Lim, J. K., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, Y., Lobodenko, A., Lokajicek, M., de Sa, R. Lopes, Luna-Garcia, R., Lyon, A. L., Maciel, A. K. A., Madar, R., Magaña-Villalba, R., Malyshev, V. L., Mansour, J., Martínez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Miconi, F., Mondal, N. K., Montgomery, H. E., Mulhearn, M., Nagy, E., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Neustroev, P., Nguyen, H. T., Nunnemann, T., Orduna, J., Osman, N., Osta, J., Pal, A., Parashar, N., Parihar, V., Park, S. K., Partridge, R., Parua, N., Patwa, A., Penning, B., Perfilov, M., Peters, Y., Petridis, K., Petrillo, G., Pétroff, P., Pleier, M. -A., Podstavkov, V. M., Popov, A. V., Prewitt, M., Price, D., Prokopenko, N., Qian, J., Quadt, A., Quinn, B., Ratoff, P. N., Razumov, I., Ripp-Baudot, I., Rizatdinova, F., Rominsky, M., Ross, A., Royon, C., Rubinov, P., Ruchti, R., Sajot, G., Sánchez-Hernández, A., Sanders, M. P., Santos, A. S., Savage, G., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schwanenberger, C., Schwienhorst, R., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shaw, S., Shchukin, A. A., Simak, V., Skubic, P., Slattery, P., Smirnov, D., Snow, G. R., Snow, J., Snyder, S., Söldner-Rembold, S., Sonnenschein, L., Soustruznik, K., Stark, J., Stoyanova, D. A., Strauss, M., Suter, L., Svoisky, P., Titov, M., Tokmenin, V. V., Tsai, Y. -T., Tsybychev, D., Tuchming, B., Tully, C., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Verkheev, A. Y., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vokac, P., Wahl, H. D., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weichert, J., Welty-Rieger, L., Williams, M. R. J., Wilson, G. W., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Yacoob, S., Yamada, R., Yang, S., Yasuda, T., Yatsunenko, Y. A., Ye, W., Ye, Z., Yin, H., Yip, K., Youn, S. W., Yu, J. M., Zennamo, J., Zhao, T. G., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We summarize and combine direct measurements of the mass of the $W$ boson in $\sqrt{s} = 1.96 \text{TeV}$ proton-antiproton collision data collected by CDF and D0 experiments at the Fermilab Tevatron Collider. Earlier measurements from CDF and D0 are combined with the two latest, more precise measurements: a CDF measurement in the electron and muon channels using data corresponding to $2.2 \mathrm{fb}^{-1}$ of integrated luminosity, and a D0 measurement in the electron channel using data corresponding to $4.3 \mathrm{fb}^{-1}$ of integrated luminosity. The resulting Tevatron average for the mass of the $W$ boson is $\MW = 80\,387 \pm 16 \text{MeV}$. Including measurements obtained in electron-positron collisions at LEP yields the most precise value of $\MW = 80\,385 \pm 15 \text{MeV}$., Comment: Submitted to Phys. Rev. D
Published: 2013
Full Text: View/download PDF

24. Detection of the compressed primary stellar wind in eta Carinae

Author: Teodoro, M., Madura, T. I., Gull, T. R., Corcoran, M. F., and Hamaguchi, K.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: A series of three HST/STIS spectroscopic mappings, spaced approximately one year apart, reveal three partial arcs in [Fe II] and [Ni II] emissions moving outward from eta Carinae. We identify these arcs with the shell-like structures, seen in the 3D hydrodynamical simulations, formed by compression of the primary wind by the secondary wind during periastron passages., Comment: Accepted for publication in the Astrophysical Journal Letters
Published: 2013
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25. Mu2e Conceptual Design Report

Author: Project, The Mu2e, Collaboration, Abrams, R. J., Alezander, D., Ambrosio, G., Andreev, N., Ankenbrandt, C. M., Asner, D. M., Arnold, D., Artikov, A., Barnes, E., Bartoszek, L., Bernstein, R. H., Biery, K., Biliyar, V., Bonicalzi, R., Bossert, R., Bowden, M., Brandt, J., Brown, D. N., Budagov, J., Buehler, M., Burov, A., Carcagno, R., Carey, R. M., Carosi, R., Cascella, M., Cauz, D., Cervelli, F., Chandra, A., Chang, J. K., Cheng, C., Ciambrone, P., Coleman, R. N., Cooper, M., Corcoran, M. C., Cordelli, M., Davydov, Y., de Gouvea, A. L., De Lorenzis, L., Debevec, P. T., DeJongh, F., Densham, C., Deuerling, G., Dey, J., Di Falco, S., Dixon, S., Djilkibaev, R., Drendel, B., Dukes, E. C., Dychkant, A., Echenard, B., Ehrlich, R., Evans, N., Evbota, D., Fang, I., Fast, J. E., Feher, S., Fischler, M., Frank, M., Frlez, E., Fung, S. S., Gallo, G., Galucci, G., Gaponenko, A., Genser, K., Giovannella, S., Glagolev, V., Glenzinski, D., Gnani, D., Goadhouse, S., Gollin, G. D., Grace, C., Grancagnolo, F., Group, C., Hanson, J., Hanson, S., Happacher, F., Heckmaier, E., Hedin, D., Hertzog, D. W., Hirosky, R., Hitlin, D. G., Ho, E., Huang, X., Huedem, E., Hung, P. Q., Hungerford, E. V., Ito, T., Jaskierny, W., Jedziniak, R., Johnson, R. P., Johnstone, C., Johnstone, J. A., Kahn, S. A., Kammel, P., Kang, T. I., Kashikhin, V. S., Kashikhin, V. V., Kasper, P., Kawall, D. M., Khalatian, V., Kim, M., Klebaner, A., Kocen, D., Kolomensky, Y., Kourbanis, I., Kowalkowski, J., Kozminski, J., Krempetz, K., Kumar, K. S., Kutschke, R. K., Kwarciany, R., Lackowski, T., Lamm, M., Larwill, M., Lau, K., Lee, M. J., L'Erario, A., Leveling, T., Lim, G., Lindenmeyer, C., Logashenko, V., Lontadze, T., Lopes, M., Luca, A., Lynch, K. R., Ma, T., Maffezzoli, A., Marciano, W. J., Martini, M., Masayoshi, W., Matushko, V., McAteer, M., McCrady, R., Moccoli, A., Michelotti, L., Miller, J. P., Miscetti, S., Molzon, W., Morgan, J., Mukherjee, A., Nagaitsev, S., Nagaslaev, V., Niehoff, J., Neuffer, D. V., Nicol, T., Norman, A. J., Norris, B., Odell, J., Oh, S., Oksuzian, Y., Onorato, G., Orduna, J., Orris, D., Ostojic, R., Page, T., Paschke, K. D., Pauletta, G., Peterson, T., Piacentino, G. M., Pileggi, G., Pla-Dalmau, A., Pocanic, D., Polly, C. C., Polychronakos, V., Ponzio, B., Popovic, M., Popp, J. L., Porter, F., Presbys, E., Prieto, P., Pronskikh, V., Puccinelli, F., Rabehl, R., Ramsey, J., Ray, R. E., Rechenmacher, R., Rella, S., Ristori, L., Rivera, R., Roberts, B. L., Roberts, T. J., Rubinov, P., Rusu, V. L., Saputi, A., Sarra, I., Smertzidis, Y., Shanahan, P., Simonenko, A., Steward, J., Suslov, I., Sylvester, C., Tang, Z., Tartaglia, M., Tassielli, G., Tereshchenko, V., Theilacker, J., Tompkins, J., Tschirhart, R., Van Zandbergen, G., Vannini, C., Venanzoni, G., von der Lippe, H., Wagner, R., Walder, J. P., Walton, R., Wands, S., Wang, S., Warren, G., Werkema, S., White Jr, H. B., Wielgos, R., Wood, L. S., Woodward, M., Wu, J., Xiao, M., Yamada, R., Yamin, P., Yarritu, K., Yonehara, K., Yoshikawa, C., You, Z., Yu, G., Yurkewicz, A., Zavarise, G., and Zhu, R. Y.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment, Physics - Accelerator Physics
Abstract: Mu2e at Fermilab will search for charged lepton flavor violation via the coherent conversion process mu- N --> e- N with a sensitivity approximately four orders of magnitude better than the current world's best limits for this process. The experiment's sensitivity offers discovery potential over a wide array of new physics models and probes mass scales well beyond the reach of the LHC. We describe herein the conceptual design of the proposed Mu2e experiment. This document was created in partial fulfillment of the requirements necessary to obtain DOE CD-1 approval, which was granted July 11, 2012., Comment: 562 pages, 339 figures
Published: 2012

26. Combination of the top-quark mass measurements from the Tevatron collider

Author: CDF, The, collaborations, D0, Aaltonen, T., Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Alton, A., Gonzalez, B. Alvarez, Alverson, G., Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Askew, A., Atkins, S., Auerbach, B., Augsten, K., Aurisano, A., Avila, C., Azfar, F., Badaud, F., Badgett, W., Bae, T., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barbaro-Galtieri, A., Barberis, E., Baringer, P., Barnes, V. E., Barnett, B. A., Barria, P., Bartlett, J. F., Bartos, P., Bassler, U., Bauce, M., Bazterra, V., Bean, A., Bedeschi, F., Begalli, M., Behari, S., Bellantoni, L., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besancon, M., Beuselinck, R., Bhat, P. C., Bhatia, S., Bhatnagar, V., Bhatti, A., Bisello, D., Bizjak, I., Bland, K. R., Blazey, G., Blessing, S., Bloom, K., Blumenfeld, B., Bocci, A., Bodek, A., Boehnlein, A., Boline, D., Boos, E. E., Borissov, G., Bortoletto, D., Bose, T., Boudreau, J., Boveia, A., Brandt, A., Brandt, O., Brock, L. Brigliadori R., Bromberg, C., Bross, A., Brown, D., Brown, J., Brucken, E., Bu, X. B., Budagov, J., Budd, H. S., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Burkett, K., Busetto, G., Bussey, P., Buszello, C. P., Buzatu, A., Calamba, A., Calancha, C., Camacho-Perez, E., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Casey, B. C. K., Castilla-Valdez, H., Castro, A., Catastini, P., Caughron, S., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chapon, E., Chen, G., Chen, Y. C., Chertok, M., Chevalier-Thery, S., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, D. K., Cho, K., Cho, S. W., Choi, S., Chokheli, D., Choudhary, B., Chung, W. H., Chung, Y. S., Cihangir, S., Ciocci, M. A., Claes, D., Clark, A., Clarke, C., Clutter, J., Compostella, G., Convery, M. E., Conway, J., Cooke, M., Cooper, W. E., Corbo, M., Corcoran, M., Cordelli, M., Couderc, F., Cousinou, M. -C., Cox, C. A., Cox, D. J., Crescioli, F., Croc, A., Cuevas, J., Culbertson, R., Cutts, D., Dagenhart, D., Das, A., d'Ascenzo, N., Datta, M., Davies, G., de Barbaro, P., de Jong, S. J., De La Cruz-Burelo, E., Deliot, F., Dell'Orso, M., Demina, R., Demortier, L., Deninno, M., Denisov, D., Denisov, S. P., d'Errico, M., Desai, S., Deterre, C., DeVaughan, K., Devoto, F., Di Canto, A., Di Ruzza, B., Diehl, H. T., Diesburg, M., Ding, P. F., Dittmann, J. R., Dominguez, A., Donati, S., Dong, P., D'Onofrio, M., Dorigo, M., Dorigo, T., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Ebina, K., Edmunds, D., Elagin, A., Ellison, J., Elvira, V. D., Enari, Y., Eppig, A., Erbacher, R., Errede, S., Ershaidat, N., Eusebi, R., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Farrington, S., Feindt, M., Feng, L., Ferbel, T., Fernandez, J. P., Fiedler, F., Field, R., Filthaut, F., Fisher, W., Fisk, H. E., Flanagan, G., Forrest, R., Fortner, M., Fox, H., Frank, M. J., Franklin, M., Freeman, J. C., Fuess, S., Funakoshi, Y., Furic, I., Gallinaro, M., Garcia, J. E., Garcia-Bellido, A., Garcia-Gonzalez, J. A., Garcia-Guerra, G. A., Garfinkel, A. F., Garosi, P., Gavrilov, V., Gay, P., Geng, W., Gerbaudo, D., Gerber, C. E., Gerberich, H., Gerchtein, E., Gershtein, Y., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Ginther, G., Giokaris, N., Giromini, P., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Golovanov, G., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Grenier, G., Grinstein, S., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grosso-Pilcher, C., Group, R. C., Grunendahl, S., Grunewald, M. W., Guillemin, T., da Costa, J. Guimaraes, Gutierrez, G., Gutierrez, P., Hagopian, S., Hahn, S. R., Haley, J., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Han, L., Happacher, F., Hara, K., Harder, K., Hare, D., Hare, M., Harel, A., Harr, R. F., Hatakeyama, K., Hauptman, J. M., Hays, C., Hays, J., Head, T., Hebbeker, T., Heck, M., Hedin, D., Hegab, H., Heinrich, J., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herndon, M., Herner, K., Hesketh, G., Hewamanage, S., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hocker, A., Hoeneisen, B., Hogan, J., Hohlfeld, M., Hopkins, W., Horn, D., Hou, S., Howley, I., Hubacek, Z., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Hynek, V., Iashvili, I., Ilchenko, Y., Illingworth, R., Introzzi, G., Iori, M., Ito, A. S., Ivanov, A., Jabeen, S., Jaffre, M., James, E., Jang, D., Jayasinghe, A., Jayatilaka, B., Jeon, E. J., Jeong, M. S., Jesik, R., Jindariani, S., Johns, K., Johnson, E., Johnson, M., Jonckheere, A., Jones, M., Jonsson, P., Joo, K. K., Joshi, J., Jun, S. Y., Jung, A. W., Junk, T. R., Juste, A., Kaadze, K., Kajfasz, E., Kamon, T., Karchin, P. E., Karmanov, D., Kasmi, A., Kasper, P. A., Kato, Y., Katsanos, I., Kehoe, R., Kermiche, S., Ketchum, W., Keung, J., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. J., Kim, Y. K., Kimura, N., Kirby, M., Kiselevich, I., Klimenko, S., Knoepfel, K., Kohli, J. M., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kozelov, A. V., Kraus, J., Kreps, M., Kroll, J., Krop, D., Kruse, M., Krutelyov, V., Kuhr, T., Kulikov, S., Kumar, A., Kupco, A., Kurata, M., Kurca, T., Kuzmin, V. A., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lammers, S., Lancaster, M., Lander, R. L., Landsberg, G., Lannon, K., Lath, A., Latino, G., Lebrun, P., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Lee, W. M., Lei, X., Lellouch, J., Leo, S., Leone, S., Lewis, J. D., Li, H., Li, L., Li, Q. Z., Lim, J. K., Limosani, A., Lin, C. -J., Lincoln, D., Lindgren, M., Linnemann, J., Lipaev, V. V., Lipeles, E., Lipton, R., Lister, A., Litvintsev, D. O., Liu, C., Liu, H., Liu, Q., Liu, T., Liu, Y., Lobodenko, A., Lockwitz, S., Loginov, A., Lokajicek, M., de Sa, R. Lopes, Lubatti, H. J., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Luna-Garcia, R., Lungu, G., Lyon, A. L., Lys, J., Lysak, R., Maciel, A. K. A., Madar, R., Madrak, R., Maeshima, K., Maestro, P., Magana-Villalba, R., Malik, S., Malyshev, V. L., Manca, G., Manousakis-Katsikakis, A., Maravin, Y., Margaroli, F., Marino, C., Martinez, M., Martinez-Ortega, J., Mastrandrea, P., Matera, K., Mattson, M. E., Mazzacane, A., Mazzanti, P., McCarthy, R., McFarland, K. S., McGivern, C. L., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Miao, T., Miconi, F., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondal, N. K., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Mulhearn, M., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nagy, E., Naimuddin, M., Nakano, I., Napier, A., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Nett, J., Neu, C., Neubauer, M. S., Neustroev, P., Nielsen, J., Nodulman, L., Noh, S. Y., Norniella, O., Nunnemann, T., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Orduna, J., Ortolan, L., Osman, N., Osta, J., Padilla, M., Griso, S. Pagan, Pagliarone, C., Pal, A., Palencia, E., Papadimitriou, V., Paramonov, A. A., Parashar, N., Parihar, V., Park, S. K., Partridge, R., Parua, N., Patrick, J., Patwa, A., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penning, B., Penzo, A., Perfilov, M., Peters, Y., Petridis, K., Petrillo, G., Petroff, P., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pleier, M. -A., Podesta-Lerma, P. L. M., Podstavkov, V. M., Pondrom, L., Popov, A. V., Poprocki, S., Potamianos, K., Pranko, A., Prewitt, M., Price, D., Prokopenko, N., Prokoshin, F., Ptohos, F., Punzi, G., Qian, J., Quadt, A., Quinn, B., Rahaman, A., Ramakrishnan, V., Rangel, M. S., Ranjan, K., Ranjan, N., Ratoff, P. N., Razumov, I., Redondo, I., Renkel, P., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ripp-Baudot, I., Ristori, L., Rizatdinova, F., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Rominsky, M., Roser, R., Ross, A., Royon, C., Rubinov, P., Ruchti, R., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sajot, G., Sakumoto, W. K., Sakurai, Y., Salcido, P., Sanchez-Hernandez, A., Sanders, M. P., Santi, L., Santos, A. S., Sato, K., Savage, G., Saveliev, V., Savoy-Navarro, A., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schlabach, P., Schlobohm, S., Schmidt, A., Schmidt, E. E., Schwanenberger, C., Schwarz, T., Schwienhorst, R., Scodellaro, L., Scribano, A., Scuri, F., Seidel, S., Seiya, Y., Sekaric, J., Semenov, A., Severini, H., Sforza, F., Shabalina, E., Shalhout, S. Z., Shary, V., Shaw, S., Shchukin, A. A., Shears, T., Shepard, P. F., Shimojima, M., Shivpuri, R. K., Shochet, M., Shreyber-Tecker, I., Simak, V., Simonenko, A., Sinervo, P., Skubic, P., Slattery, P., Sliwa, K., Smirnov, D., Smith, J. R., Smith, K. J., Snider, F. D., Snow, G. R., Snow, J., Snyder, S., Soha, A., Soldner-Rembold, S., Song, H., Sonnenschein, L., Sorin, V., Soustruznik, K., Squillacioti, P., Denis, R. St., Stancari, M., Stark, J., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Stoyanova, D. A., Strauss, M., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Suter, L., Svoisky, P., Takahashi, M., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Titov, M., Toback, D., Tokar, S., Tokmenin, V. V., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tsai, Y. -T., Tschann-Grimm, K., Tsybychev, D., Tuchming, B., Tully, C., Ukegawa, F., Uozumi, S., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varganov, A., Varnes, E. W., Vasilyev, I. A., Vazquez, F., Velev, G., Vellidis, C., Verdier, P., Verkheev, A. Y., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vidal, M., Vila, I., Vilanova, D., Vilar, R., Vizan, J., Vogel, M., Vokac, P., Volpi, G., Wagner, P., Wagner, R. L., Wahl, H. D., Wakisaka, T., Wallny, R., Wang, M. H. L. S., Wang, S. M., Warburton, A., Warchol, J., Waters, D., Watts, G., Wayne, M., Weichert, J., Welty-Rieger, L., Wester III, W. C., White, A., Whiteson, D., Wick, F., Wicke, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Williams, H. H., Williams, M. R. J., Wilson, G. W., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wobisch, M., Wolbers, S., Wolfe, H., Wood, D. R., Wright, T., Wu, X., Wu, Z., Wyatt, T. R., Xie, Y., Yamada, R., Yamamoto, K., Yamato, D., Yang, S., Yang, T., Yang, U. K., Yang, W. -C., Yang, Y. C., Yao, W. -M., Yasuda, T., Yatsunenko, Y. A., Ye, W., Ye, Z., Yeh, G. P., Yin, H., Yi, K., Yip, K., Yoh, J., Yorita, K., Yoshida, T., Youn, S. W., Yu, G. B., Yu, I., Yu, J. M., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., Zennamo, J., Zhao, T., Zhao, T. G., Zhou, B., Zhou, C., Zhu, J., Zielinski, M., Zieminska, D., Zivkovic, L., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: The top quark is the heaviest known elementary particle, with a mass about 40 times larger than the mass of its isospin partner, the bottom quark. It decays almost 100% of the time to a $W$ boson and a bottom quark. Using top-antitop pairs at the Tevatron proton-antiproton collider, the CDF and {\dzero} collaborations have measured the top quark's mass in different final states for integrated luminosities of up to 5.8 fb$^{-1}$. This paper reports on a combination of these measurements that results in a more precise value of the mass than any individual decay channel can provide. It describes the treatment of the systematic uncertainties and their correlations. The mass value determined is $173.18 \pm 0.56 \thinspace ({\rm stat}) \pm 0.75 \thinspace ({\rm syst})$ GeV or $173.18 \pm 0.94$ GeV, which has a precision of $\pm 0.54%$, making this the most precise determination of the top quark mass., Comment: 30 pages and 6 figures, published in Phys. Rev. D
Published: 2012
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27. Measurement of the differential cross section d\sigma/dt in elastic $p\bar{p}$ scattering at sqrt(s)=1.96 TeV

Author: D0 Collaboration, Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Alton, A., Alverson, G., Alves, G. A., Aoki, M., Askew, A., Atkins, S., Augsten, K., Avila, C., Badaud, F., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Barreto, J., Bartlett, J. F., Bassler, U., Bazterra, V., Bean, A., Begalli, M., Bellantoni, L., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besançon, M., Beuselinck, R., Bezzubov, V. A., Bhat, P. C., Bhatia, S., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Boos, E. E., Borissov, G., Bose, T., Brandt, A., Brandt, O., Brock, R., Brooijmans, G., Bross, A., Brown, D., Brown, J., Bu, X. B., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Buszello, C. P., Camacho-Pérez, E., Carvalho, W., Casey, B. C. K., Castilla-Valdez, H., Caughron, S., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chapon, E., Chen, G., Chevalier-Théry, S., Cho, D. K., Cho, S. W., Choi, S., Choudhary, B., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Croc, A., Cutts, D., Das, A., Davies, G., de Jong, S. J., De La Cruz-Burelo, E., Martins, C. De Oliveira, Déliot, F., Demina, R., Denisov, D., Denisov, S. P., Desai, S., Deterre, C., DeVaughan, K., Diehl, H. T., Diesburg, M., Ding, P. F., Dominguez, A., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Edmunds, D., Ellison, J., Elvira, V. D., Enari, Y., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Feng, L., Ferbel, T., Fiedler, F., Filthaut, F., Fisher, W., Fisk, H. E., Fortner, M., Fox, H., Fuess, S., Garcia-Bellido, A., García-González, J. A., García-Guerra, G. A., Gavrilov, V., Gay, P., Geng, W., Gerbaudo, D., Gerber, C. E., Gershtein, Y., Ginther, G., Golovanov, G., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Gregores, E. M., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grünendahl, S., Grünewald, M. W., Guillemin, T., Gutierrez, G., Gutierrez, P., Haas, A., Hagopian, S., Haley, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hohlfeld, M., Howley, I., Hubacek, Z., Hynek, V., Iashvili, I., Ilchenko, Y., Illingworth, R., Ito, A. S., Jabeen, S., Jaffré, M., Jayasinghe, A., Jesik, R., Johns, K., Johnson, E., Johnson, M., Jonckheere, A., Jonsson, P., Joshi, J., Jung, A. W., Juste, A., Kaadze, K., Kajfasz, E., Karmanov, D., Kasper, P. A., Katsanos, I., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Kiselevich, I., Kohli, J. M., Kozelov, A. V., Kraus, J., Kulikov, S., Kumar, A., Kupco, A., Kurča, T., Kuzmin, V. A., Lammers, S., Landsberg, G., Lebrun, P., Lee, H. S., Lee, S. W., Lee, W. M., Lellouch, J., Li, H., Li, L., Li, Q. Z., Lim, J. K., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, H., Liu, Y., Lobodenko, A., Lokajicek, M., de Sa, R. Lopes, Lubatti, H. J., Luna-Garcia, R., Lyon, A. L., Maciel, A. K. A., Madar, R., Magaña-Villalba, R., Malik, S., Malyshev, V. L., Maravin, Y., Martínez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Mendoza, L., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Miconi, F., Molina, J., Mondal, N. K., da Motta, H., Mulhearn, M., Mundim, L., Nagy, E., Naimuddin, M., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Neustroev, P., Novaes, S. F., Nunnemann, T., Obrant, G., Oguri, V., Orduna, J., Osman, N., Osta, J., Padilla, M., Pal, A., Parashar, N., Parihar, V., Park, S. K., Partridge, R., Parua, N., Patwa, A., Penning, B., Perfilov, M., Peters, Y., Petridis, K., Petrillo, G., Pétroff, P., Pleier, M. -A., Podesta-Lerma, P. L. M., Podstavkov, V. M., Pol, M. -E., Popov, A. V., da Silva, W. L. Prado, Prewitt, M., Price, D., Prokopenko, N., Qian, J., Quadt, A., Quinn, B., Rangel, M. S., Ranjan, K., Ratoff, P. N., Razumov, I., Renkel, P., Ripp-Baudot, I., Rizatdinova, F., Rominsky, M., Ross, A., Royon, C., Rubinov, P., Ruchti, R., Sajot, G., Salcido, P., Sánchez-Hernández, A., Sanders, M. P., Sanghi, B., Santoro, A., Santos, A. S., Savage, G., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schlobohm, S., Schwanenberger, C., Schwienhorst, R., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shaw, S., Shchukin, A. A., Shivpuri, R. K., Simak, V., Skubic, P., Slattery, P., Smirnov, D., Smith, K. J., Snow, G. R., Snow, J., Snyder, S., Söldner-Rembold, S., Sonnenschein, L., Soustruznik, K., Stark, J., Stoyanova, D. A., Strang, M. A., Strauss, M., Stutte, L., Suter, L., Svoisky, P., Takahashi, M., Titov, M., Tokmenin, V. V., Tsai, Y. -T., Tschann-Grimm, K., Tsybychev, D., Tuchming, B., Tully, C., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Verdier, P., Verkheev, A. Y., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vokac, P., Wahl, H. D., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weichert, J., Welty-Rieger, L., White, A., Wicke, D., Williams, M. R. J., Wilson, G. W., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Yamada, R., Yang, W. -C., Yasuda, T., Yatsunenko, Y. A., Ye, W., Ye, Z., Yin, H., Yip, K., Youn, S. W., Zennamo, J., Zhao, T., Zhao, T. G., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We present a measurement of the elastic differential cross section $d\sigma(p\bar{p}\rightarrow p\bar{p})/dt$ as a function of the four-momentum-transfer squared t. The data sample corresponds to an integrated luminosity of $\approx 31 nb^{-1}$ collected with the D0 detector using dedicated Tevatron $p\bar{p} $ Collider operating conditions at sqrt(s) = 1.96 TeV and covers the range $0.26 <|t|< 1.2 GeV^2$. For $|t|<0.6 GeV^2$, d\sigma/dt is described by an exponential function of the form $Ae^{-b|t|}$ with a slope parameter $ b = 16.86 \pm 0.10(stat) \pm 0.20(syst) GeV^{-2}$. A change in slope is observed at $|t| \approx 0.6 GeV^2$, followed by a more gradual |t| dependence with increasing values of |t|., Comment: 12 pages, 12 figures, 1 table, submitted to Phys. Rev. D, FERMILAB-PUB-12-263-E
Published: 2012
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28. The D0 Run IIb Luminosity Measurement

Author: Casey, B. C. K., Corcoran, M., DeVaughan, K., Enari, Y., Gallas, E., Katsanos, I., Linnemann, J., Orduna, J., Partridge, R., Prewitt, M., Schellman, H., Snow, G. R., and Verzocchi, M.
Subjects: High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract: An assessment of the recorded integrated luminosity is presented for data collected with the D0 detector at the Fermilab Tevatron Collider from June 2006 to September 2011 (Run IIb). In addition, a measurement of the effective cross section for inelastic interactions, also referred to as the luminosity constant, is reported. This measurement incorporates new features that lead to a substantial improvement in the precision of the result. A luminosity constant of \sigma_{LM} = 48.3\pm1.9\pm0.6 mb is obtained, where the first uncertainty is due to the accuracy of the inelastic cross section used by both CDF and D0, and the second uncertainty is due to D0 sources. The recorded luminosity for the highest E_T jet trigger is L_rec = 9.2 \pm 0.4 fb^{-1}, with a relative uncertainty of 4.3%., Comment: 20 pages, 23 figures
Published: 2012
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29. Combination of CDF and D0 measurements of the W boson helicity in top quark decays

Author: CDF, The, Collaborations, D0, Aaltonen, T., Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Alton, A., González, B. Álvarez, Alverson, G., Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Aoki, M., Apollinari, G., Appel, J. A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Askew, A., Åsman, B., Atkins, S., Atramentov, O., Auerbach, B., Augsten, K., Aurisano, A., Avila, C., Azfar, F., Badaud, F., Badgett, W., Bae, T., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barbaro-Galtieri, A., Barberis, E., Baringer, P., Barnes, V. E., Barnett, B. A., Barreto, J., Barria, P., Bartlett, J. F., Bartos, P., Bassler, U., Bauce, M., Bazterra, V., Bean, A., Bedeschi, F., Begalli, M., Behari, S., Belanger-Champagne, C., Bellantoni, L., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besançon, M., Beuselinck, R., Bezzubov, V. A., Bhatia, S., Bhatnagar, V., Bhatti, A., Bhat, P. C., Bisello, D., Bizjak, I., Bland, K. R., Blazey, G., Blessing, S., Bloom, K., Blumenfeld, B., Bocci, A., Bodek, A., Boehnlein, A., Boline, D., Boos, E. E., Borissov, G., Bortoletto, D., Bose, T., Boudreau, J., Boveia, A., Brandt, A., Brandt, O., Brigliadori, L., Brock, R., Bromberg, C., Brooijmans, G., Bross, A., Brown, D., Brown, J., Brucken, E., Bu, X. B., Budagov, J., Budd, H. S., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Burkett, K., Bussey, P., Buszello, C. P., Buzatu, A., Calamba, A., Calancha, C., Camacho-Pérez, E., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Casey, B. C. K., Castilla-Valdez, H., Castro, A., Catastini, P., Caughron, S., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chapon, E., Chen, Y. C., Chen, G., Chertok, M., Chevalier-Théry, S., Chiarelli, G., Chlachidze, G., Chlebana, F., Choi, S., Chokheli, D., Choudhary, B., Cho, D. K., Cho, K., Cho, S. W., Chung, W. H., Chung, Y. S., Cihangir, S., Ciocci, M. A., Claes, D., Clarke, C., Clark, A., Clutter, J., Compostella, G., Convery, M. E., Conway, J., Cooke, M., Cooper, W. E., Corbo, M., Corcoran, M., Cordelli, M., Couderc, F., Cousinou, M. -C., Cox, C. A., Cox, D. J., Crescioli, F., Croc, A., Cuevas, J., Culbertson, R., Cutts, D., d'Ascenzo, N., d'Errico, M., D'Onofrio, M., Dagenhart, D., Das, A., Datta, M., Davies, G., Déliot, F., Dell'Orso, M., Demina, R., Demortier, L., Deninno, M., Denisov, D., Denisov, S. P., Desai, S., Deterre, C., DeVaughan, K., Devoto, F., de Barbaro, P., de Jong, S. J., De La Cruz-Burelo, E., Diehl, H. T., Diesburg, M., Ding, P. F., Dittmann, J. R., Di Canto, A., Di Ruzza, B., Dominguez, A., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Dorland, T., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Ebina, K., Edmunds, D., Elagin, A., Ellison, J., Elvira, V. D., Enari, Y., Eppig, A., Erbacher, R., Errede, S., Ershaidat, N., Eusebi, R., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Farrington, S., Feindt, M., Ferbel, T., Feng, L., Fernandez, J. P., Fiedler, F., Field, R., Filthaut, F., Fisher, W., Fisk, H. E., Flanagan, G., Forrest, R., Fortner, M., Fox, H., Franklin, M., Frank, M. J., Freeman, J. C., Fuess, S., Funakoshi, Y., Furic, I., Gallinaro, M., Garcia, J. E., Garcia-Bellido, A., García-Guerra, G. A, Garfinkel, A. F., Garosi, P., Gavrilov, V., Gay, P., Geng, W., Gerbaudo, D., Gerber, C. E., Gerberich, H., Gerchtein, E., Gershtein, Y., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Ginther, G., Giokaris, N., Giromini, P., Giurgiu, G., Glagolev, V., Glenzinski, D., Goldin, D., Gold, M., Goldschmidt, N., Golossanov, A., Golovanov, G., Gomez-Ceballos, G., Gomez, G., Goncharov, M., González, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Grenier, G., Grinstein, S., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grosso-Pilcher, C., Group, R. C., Grünendahl, S., Grünewald, M. W., Guillemin, T., da Costa, J. Guimaraes, Guo, F., Gutierrez, G., Gutierrez, P., Haas, A., Hagopian, S., Hahn, S. R., Haley, J., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Han, L., Happacher, F., Hara, K., Harder, K., Hare, D., Hare, M., Harel, A., Harr, R. F., Hatakeyama, K., Hauptman, J. M., Hays, C., Hays, J., Head, T., Hebbeker, T., Heck, M., Hedin, D., Hegab, H., Heinrich, J., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herndon, M., Herner, K., Hesketh, G., Hewamanage, S., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hocker, A., Hoeneisen, B., Hohlfeld, M., Hopkins, W., Horn, D., Hou, S., Howley, I., Hubacek, Z., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Hynek, V., Iashvili, I., Ilchenko, Y., Illingworth, R., Introzzi, G., Iori, M., Ito, A. S., Ivanov, A., Jabeen, S., Jaffré, M., James, E., Jamin, D., Jang, D., Jayasinghe, A., Jayatilaka, B., Jeon, E. J., Jesik, R., Jindariani, S., Johns, K., Johnson, M., Jonckheere, A., Jones, M., Jonsson, P., Joo, K. K., Joshi, J., Jun, S. Y., Jung, A. W., Junk, T. R., Juste, A., Kaadze, K., Kajfasz, E., Kamon, T., Karchin, P. E., Karmanov, D., Kasmi, A., Kasper, P. A., Kato, Y., Katsanos, I., Kehoe, R., Kermiche, S., Ketchum, W., Keung, J., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Khotilovich, V., Kilminster, B., Kimura, N., Kim, D. H., Kim, H. S., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. J., Kim, Y. K., Klimenko, S., Knoepfel, K., Kohli, J. M., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kozelov, A. V., Kraus, J., Kreps, M., Kroll, J., Krop, D., Kruse, M., Krutelyov, V., Kuhr, T., Kulikov, S., Kumar, A., Kupco, A., Kurata, M., Kurča, T., Kuzmin, V. A., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lammers, S., Lancaster, M., Lander, R. L., Landsberg, G., Lannon, K., Lath, A., Latino, G., Lebrun, P., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, W. M., Lee, S. W., Lellouch, J., Leo, S., Leone, S., Lewis, J. D., Li, H., Li, L., Li, Q. Z., Lim, J. K., Limosani, A., Lin, C. -J., Lincoln, D., Lindgren, M., Linnemann, J., Lipaev, V. V., Lipeles, E., Lipton, R., Lister, A., Litvintsev, D. O., Liu, C., Liu, H., Liu, T., Liu, Q., Liu, Y., Lobodenko, A., Lockwitz, S., Loginov, A., Lokajicek, M., de Sa, R. Lopes, Lubatti, H. J., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Luna-Garcia, R., Lungu, G., Lyon, A. L., Lysak, R., Lys, J., Maciel, A. K. A., Mackin, D., Madar, R., Madrak, R., Maeshima, K., Maestro, P., Magaña-Villalba, R., Malik, S., Malyshev, V. L., Manca, G., Manousakis-Katsikakis, A., Maravin, Y., Margaroli, F., Marino, C., Martínez, M., Martínez-Ortega, J., Mastrandrea, P., Matera, K., Mattson, M. E., Mazzacane, A., Mazzanti, P., McCarthy, R., McFarland, K. S., McGivern, C. L., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Mesropian, C., Meyer, A., Meyer, J., Miao, T., Miconi, F., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondal, N. K., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Mulhearn, M., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nagy, E., Naimuddin, M., Nakano, I., Napier, A., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Nett, J., Neubauer, M. S., Neustroev, P., Neu, C., Nielsen, J., Nodulman, L., Noh, S. Y., Norniella, O., Nunnemann, T., Oakes, L., Obrant, G., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Orduna, J., Ortolan, L., Osman, N., Osta, J., Padilla, M., Griso, S. Pagan, Pagliarone, C., Pal, A., Palencia, E., Papadimitriou, V., Paramonov, A. A., Parashar, N., Parihar, V., Park, S. K., Partridge, R., Parua, N., Patrick, J., Patwa, A., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penning, B., Penzo, A., Perfilov, M., Peters, Y., Petridis, K., Petrillo, G., Pétroff, P., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pleier, M. -A., Podesta-Lerma, P. L. M., Podstavkov, V. M., Polozov, P., Pondrom, L., Popov, A. V., Poprocki, S., Potamianos, K., Prewitt, M., Price, D., Prokopenko, N., Prokoshin, F., Pranko, A., Ptohos, F., Punzi, G., Qian, J., Quadt, A., Quinn, B., Rahaman, A., Ramakrishnan, V., Rangel, M. S., Ranjan, K., Ranjan, N., Ratoff, P. N., Razumov, I., Redondo, I., Renkel, P., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ripp-Baudot, I., Ristori, L., Rizatdinova, F., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Rominsky, M., Roser, R., Ross, A., Royon, C., Rubinov, P., Ruchti, R., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Safronov, G., Sajot, G., Sakumoto, W. K., Sakurai, Y., Salcido, P., Sánchez-Hernández, A., Sanders, M. P., Sanghi, B., Santi, L., Santos, A. S., Sato, K., Savage, G., Saveliev, V., Savoy-Navarro, A., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schlabach, P., Schlobohm, S., Schmidt, A., Schmidt, E. E., Schwanenberger, C., Schwarz, T., Schwienhorst, R., Scodellaro, L., Scribano, A., Scuri, F., Seidel, S., Seiya, Y., Sekaric, J., Semenov, A., Severini, H., Sforza, F., Shabalina, E., Shalhout, S. Z., Shary, V., Shaw, S., Shchukin, A. A., Shears, T., Shepard, P. F., Shimojima, M., Shivpuri, R. K., Shochet, M., Shreyber-Tecker, I., Simak, V., Simonenko, A., Sinervo, P., Skubic, P., Slattery, P., Sliwa, K., Smirnov, D., Smith, J. R., Smith, K. J., Snider, F. D., Snow, G. R., Snow, J., Snyder, S., Soha, A., Söldner-Rembold, S., Song, H., Sonnenschein, L., Sorin, V., Soustruznik, K., Squillacioti, P., Denis, R. St., Stancari, M., Stark, J., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Stolin, V., Stoyanova, D. A., Strauss, M., Strologas, J., Strycker, G. L., Stutte, L., Sudo, Y., Sukhanov, A., Suslov, I., Suter, L., Svoisky, P., Takahashi, M., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Titov, M., Toback, D., Tokar, S., Tokmenin, V. V., Tollefson, K., Tomura, T., Tonelli, D., Torretta, D., Torre, S., Totaro, P., Trovato, M., Tsai, Y. -T., Tschann-Grimm, K., Tsybychev, D., Tuchming, B., Tully, C., Ukegawa, F., Uozumi, S., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varganov, A., Varnes, E. W., Vasilyev, I. A., Vázquez, F., Velev, G., Vellidis, C., Verdier, P., Verkheev, A. Y., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vidal, M., Vila, I., Vilanova, D., Vilar, R., Vizán, J., Vogel, M., Vokac, P., Volpi, G., Wagner, P., Wagner, R. L., Wahl, H. D., Wakisaka, T., Wallny, R., Wang, M. H. L. S., Wang, S. M., Warburton, A., Warchol, J., Waters, D., Watts, G., Wayne, M., Weichert, J., Welty-Rieger, L., Wester III, W. C., White, A., Whiteson, D., Wick, F., Wicke, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Williams, H. H., Williams, M. R. J., Wilson, G. W., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wobisch, M., Wolbers, S., Wolfe, H., Wood, D. R., Wright, T., Wu, X., Wu, Z., Wyatt, T. R., Xie, Y., Yamada, R., Yamamoto, K., Yang, T., Yang, U. K., Yang, W. -C., Yang, Y. C., Yao, W. -M., Yasuda, T., Yatsunenko, Y. A., Ye, Z., Yeh, G. P., Yi, K., Yin, H., Yip, K., Yoh, J., Yorita, K., Yoshida, T., Youn, S. W., Yu, I., Yu, G. B., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., Zhao, T., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., Zivkovic, L., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: We report the combination of recent measurements of the helicity of the W boson from top quark decay by the CDF and D0 collaborations, based on data samples corresponding to integrated luminosities of 2.7 - 5.4 fb^-1 of ppbar collisions collected during Run II of the Fermilab Tevatron Collider. Combining measurements that simultaneously determine the fractions of W bosons with longitudinal (f0) and right-handed (f+) helicities, we find f0 = 0.722 \pm 0.081 [\pm 0.062 (stat.) \pm 0.052 (syst.)] and f+ = -0.033 \pm 0.046 [\pm 0.034 (stat.) \pm 0.031 (syst.)]. Combining measurements where one of the helicity fractions is fixed to the value expected in the standard model, we find f0 = 0.682 \pm 0.057 [\pm 0.035 (stat.) \pm 0.046 (syst.)] and f+ = -0.015\pm0.035 [\pm 0.018 (stat.) \pm 0.030 (syst.)]. The results are consistent with standard model expectations., Comment: 11 pages, 1 figure, to be submitted to Phys. Rev D Rap. Comm
Published: 2012
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30. Search for pair production of the scalar top quark in muon+tau final states

Author: D0 Collaboration, Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Alton, A., Alverson, G., Aoki, M., Askew, A., Asman, B., Atkins, S., Atramentov, O., Augsten, K., Avila, C., BackusMayes, J., Badaud, F., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Barreto, J., Bartlett, J. F., Bassler, U., Bazterra, V., Bean, A., Begalli, M., Belanger-Champagne, C., Bellantoni, L., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besancon, M., Beuselinck, R., Bezzubov, V. A., Bhat, P. C., Bhatia, S., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Boos, E. E., Borissov, G., Bose, T., Brandt, A., Brandt, O., Brock, R., Brooijmans, G., Bross, A., Brown, D., Brown, J., Bu, X. B., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Burnett, T. H., Buszello, C. P., Calpas, B., Camacho-Perez, E., Carrasco-Lizarraga, M. A., Casey, B. C. K., Castilla-Valdez, H., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chapon, E., Chen, G., Chevalier-Thery, S., Cho, D. K., Cho, S. W., Choi, S., Choudhary, B., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Croc, A., Cutts, D., Das, A., Davies, G., de Jong, S. J., De La Cruz-Burelo, E., Deliot, F., Demina, R., Denisov, D., Denisov, S. P., Desai, S., Deterre, C., DeVaughan, K., Diehl, H. T., Diesburg, M., Ding, P. F., Dominguez, A., Dorland, T., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Edmunds, D., Ellison, J., Elvira, V. D., Enari, Y., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Ferbel, T., Fiedler, F., Filthaut, F., Fisher, W., Fisk, H. E., Fortner, M., Fox, H., Fuess, S., Garcia-Bellido, A., Garcia-Guerra, G. A., Gavrilov, V., Gay, P., Geng, W., Gerbaudo, D., Gerber, C. E., Gershtein, Y., Ginther, G., Golovanov, G., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Greenwood, Z. D., Gregores, E. M., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grunendahl, S., Grunewald, M. W., Guillemin, T., Gutierrez, G., Gutierrez, P., Haas, A., Hagopian, S., Haley, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hohlfeld, M., Hubacek, Z., Hynek, V., Iashvili, I., Ilchenko, Y., Illingworth, R., Ito, A. S., Jabeen, S., Jaffre, M., Jamin, D., Jayasinghe, A., Jesik, R., Johns, K., Johnson, M., Jonckheere, A., Jonsson, P., Joshi, J., Jung, A. W., Juste, A., Kaadze, K., Kajfasz, E., Karmanov, D., Kasper, P. A., Katsanos, I., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Kohli, J. M., Kozelov, A. V., Kraus, J., Kulikov, S., Kumar, A., Kupco, A., Kurca, T., Kuzmin, V. A., Lammers, S., Landsberg, G., Lebrun, P., Lee, H. S., Lee, S. W., Lee, W. M., Lellouch, J., Li, H., Li, L., Li, Q. Z., Lietti, S. M., Lim, J. K., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, Y., Lobodenko, A., Lokajicek, M., de Sa, R. Lopes, Lubatti, H. J., Luna-Garcia, R., Lyon, A. L., Maciel, A. K. A., Mackin, D., Madar, R., Magana-Villalba, R., Malik, S., Malyshev, V. L., Maravin, Y., Martinez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Miconi, F., Mondal, N. K., Muanza, G. S., Mulhearn, M., Nagy, E., Naimuddin, M., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Neustroev, P., Novaes, S. F., Nunnemann, T., Obrant, G., Orduna, J., Osman, N., Osta, J., Garzon, G. J. Otero y, Padilla, M., Pal, A., Parashar, N., Parihar, V., Park, S. K., Partridge, R., Parua, N., Patwa, A., Penning, B., Perfilov, M., Peters, Y., Petridis, K., Petrillo, G., Petroff, P., Piegaia, R., Pleier, M. -A., Podesta-Lerma, P. L. M., Podstavkov, V. M., Polozov, P., Popov, A. V., Prewitt, M., Price, D., Prokopenko, N., Qian, J., Quadt, A., Quinn, B., Rangel, M. S., Ranjan, K., Ratoff, P. N., Razumov, I., Renkel, P., Rijssenbeek, M., Ripp-Baudot, I., Rizatdinova, F., Rominsky, M., Ross, A., Royon, C., Rubinov, P., Ruchti, R., Safronov, G., Sajot, G., Salcido, P., Sanchez-Hernandez, A., Sanders, M. P., Sanghi, B., Santos, A. S., Savage, G., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schliephake, T., Schlobohm, S., Schwanenberger, C., Schwienhorst, R., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shchukin, A. A., Shivpuri, R. K., Simak, V., Sirotenko, V., Skubic, P., Slattery, P., Smirnov, D., Smith, K. J., Snow, G. R., Snow, J., Snyder, S., Soldner-Rembold, S., Sonnenschein, L., Soustruznik, K., Stark, J., Stolin, V., Stoyanova, D. A., Strauss, M., Strom, D., Stutte, L., Suter, L., Svoisky, P., Takahashi, M., Tanasijczuk, A., Titov, M., Tokmenin, V. V., Tsai, Y. -T., Tschann-Grimm, K., Tsybychev, D., Tuchming, B., Tully, C., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Verdier, P., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vokac, P., Wahl, H. D., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weber, M., Weichert, J., Welty-Rieger, L., White, A., Wicke, D., Williams, M. R. J., Wilson, G. W., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Yamada, R., Yang, W. -C., Yasuda, T., Yatsunenko, Y. A., Ye, W., Ye, Z., Yin, H., Yip, K., Youn, S. W., Zhao, T., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We present a search for the pair production of scalar top quarks ($\tilde{t}_{1}$), the lightest supersymmetric partners of the top quarks, in $p\bar{p}$ collisions at a center-of-mass energy of 1.96 TeV, using data corresponding to an integrated luminosity of {7.3 $fb^{-1}$} collected with the \dzero experiment at the Fermilab Tevatron Collider. Each scalar top quark is assumed to decay into a $b$ quark, a charged lepton, and a scalar neutrino ($\tilde{\nu}$). We investigate final states arising from $\tilde{t}_{1} \bar{\tilde{t}_{1}} \rightarrow b\bar{b}\mu\tau \tilde{\nu} \tilde{\nu}$ and $\tilde{t}_{1} \bar{\tilde{t}_{1}} \rightarrow b\bar{b}\tau\tau \tilde{\nu} \tilde{\nu}$. With no significant excess of events observed above the background expected from the standard model, we set exclusion limits on this production process in the ($m_{\tilde{t}_{1}}$,$m_{\tilde{\nu}}$) plane., Comment: Submitted to Phys. Lett. B
Published: 2012
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31. Galactic Sources Science With Agile: The Case Of The Carina Region

Author: Sabatini, S., Tavani, M., Pian, E., Bulgarelli, A., Caraveo, P., Viotti, R., Corcoran, M. F., Giuliani, A., Pittori, C., Verrecchia, F., Vercellone, S., Mereghetti, S., Argan, A., Barbiellini, G., Boffelli, F., Cattaneo, P. W., Chen, A. W., Cocco, V., D'Ammando, F., Costa, E., De Paris, G., Del Monte, E., Di Cocco, G., Donnarumma, I., Evangelista, Y., Ferrari, A., Feroci, M., Fiorini, M., Froysland, T., Fuschino, F., Galli, M., Gianotti, F., Labanti, C., Lapshov, I., Lazzarotto, F., Lipari, P., Longo, F., Marisaldi, M., Mastropietro, M., Morelli, E., Moretti, E., Morselli, A., Pacciani, L., Pellizzoni, A., Perotti, F., Piano, G., Picozza, P., Pilia, M., Porrovecchio, G., Pucella, G., Prest, M., Rapisarda, M., Rappoldi, A., Rubini, A., Soffitta, P., Trifoglio, M., Trois, A., Vallazza, E., Vittorini, V., Zambra, A., Zanello, D., Santolamazza, P., Giommi, P., Colafrancesco, S., Antonelli, L. A., and Salotti, L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: During its first 2 years of operation, the gamma-ray AGILE satellite accumulated an extensive dataset for the Galactic plane. The data have been monitored for transient sources and several gamma-ray sources were detected. Their variability and possible association were studied. In this talk we will focus on the results of extensive observations of the Carina Region during the time period 2007 July - 2009 January, for a total livetime of ~130 days. The region is extremely complex, hosting massive star formation, with the remarkable colliding wind binary Eta Carinae, massive star clusters and HII regions (e.g. NGC 3324, RCW49, Westerlund II) and a giant molecular cloud extending over 150 pc (between l=284.7 and l=289). The Carina Nebula itself is the largest and IR highest surface brightness nebula of the Southern emisphere. We monitored several gamma ray sources in the Carina Region. In particular we detect a gamma ray source (1AGL J1043-5931) consistent with the position of Eta Carinae and report a remarkable 2-days gamma-ray flaring episode from this source on 2008 Oct 11-13. If 1AGL J1043-5931 is associated with the Eta Car system, our data provides the long sought first detection above 100 MeV of a colliding wind binary., Comment: 5 pages, 5 figures, proceedings of RICAP 2009
Published: 2012
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32. Search for the Rare Decays KL->pi0pi0mu+mu- and KL->pi0pi0X0->pi0pi0mu+mu-

Author: KTeV Collaboration, Abouzaid, E., Arenton, M., Barker, A. R., Bellantoni, L., Blucher, E., Bock, G. J., Cheu, E., Coleman, R., Corcoran, M. D., Cox, B., Erwin, A. R., Escobar, C. O., Glazov, A., Golossanov, A., Gomes, R. A., Gouffon, P., Hsiung, Y. B., Jensen, D. A., Kessler, R., Kotera, K., Ledovskoy, A., McBride, P. L., Monnier, E., Nguyen, H., Niclasen, R., Phillips II, D. G., Ping, H., Ramberg, E. J., Ray, R. E., Ronquest, M., Santos, E., Slater, W., Smith, D., Solomey, N., Swallow, E. C., Toale, P. A., Tschirhart, R., Velissaris, C., Wah, Y. W., Wang, J., White, H. B., Whitmore, J., Wilking, M. J., Winston, R., Worcester, E. T., Worcester, M., Yamanaka, T., Zimmerman, E. D., and Zukanovich, R. F.
Subjects: High Energy Physics - Experiment
Abstract: The KTeV E799 experiment has conducted a search for the rare decays KL->pi0pi0mu+mu- and KL->pi0pi0X0->pi0pi0mu+mu-, where the X0 is a possible new neutral boson that was reported by the HyperCP experiment with a mass of (214.3 pm 0.5) MeV/c^{2}. We find no evidence for either decay. We obtain upper limits of Br(KL->pi0pi0X0->pi0pi0mu+mu-) < 1.0 x 10^{-10} and Br(KL->pi0pi0mu+mu-) < 9.2 x 10^{-11} at the 90% confidence level. This result rules out the pseudoscalar X0 as an explanation of the HyperCP result under the scenario that the \bar{d}sX0 coupling is completely real.
Published: 2011
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33. Precise measurement of the top quark mass in the dilepton channel at D0

Author: D0 Collaboration, Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Alton, A., Alverson, G., Alves, G. A., Ancu, L. S., Aoki, M., Arov, M., Askew, A., Åsman, B., Atramentov, O., Avila, C., BackusMayes, J., Badaud, F., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Barreto, J., Bartlett, J. F., Bassler, U., Bazterra, V., Beale, S., Bean, A., Begalli, M., Begel, M., Belanger-Champagne, C., Bellantoni, L., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besançon, M., Beuselinck, R., Bezzubov, V. A., Bhat, P. C., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Boos, E. E., Borissov, G., Bose, T., Brandt, A., Brandt, O., Brock, R., Brooijmans, G., Bross, A., Brown, D., Brown, J., Bu, X. B., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Burnett, T. H., Buszello, C. P., Calpas, B., Camacho-Pérez, E., Carrasco-Lizarraga, M. A., Casey, B. C. K., Castilla-Valdez, H., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chen, G., Chevalier-Théry, S., Cho, D. K., Cho, S. W., Choi, S., Choudhary, B., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Croc, A., Cutts, D., Das, A., Davies, G., De, K., de Jong, S. J., De La Cruz-Burelo, E., Déliot, F., Demarteau, M., Demina, R., Denisov, D., Denisov, S. P., Desai, S., Deterre, C., DeVaughan, K., Diehl, H. T., Diesburg, M., Dominguez, A., Dorland, T., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Edmunds, D., Ellison, J., Elvira, V. D., Enari, Y., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Ferbel, T., Fiedler, F., Filthaut, F., Fisher, W., Fisk, H. E., Fortner, M., Fox, H., Fuess, S., Garcia-Bellido, A., Gavrilov, V., Gay, P., Geng, W., Gerbaudo, D., Gerber, C. E., Gershtein, Y., Ginther, G., Golovanov, G., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Greenwood, Z. D., Gregores, E. M., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grünendahl, S., Grünewald, M. W., Guillemin, T., Guo, F., Gutierrez, G., Gutierrez, P., Haas, A., Hagopian, S., Haley, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hohlfeld, M., Hubacek, Z., Huske, N., Hynek, V., Iashvili, I., Illingworth, R., Ito, A. S., Jabeen, S., Jaffré, M., Jamin, D., Jayasinghe, A., Jesik, R., Johns, K., Johnson, M., Johnston, D., Jonckheere, A., Jonsson, P., Joshi, J., Jung, A. W., Juste, A., Kaadze, K., Kajfasz, E., Karmanov, D., Kasper, P. A., Katsanos, I., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Khatidze, D., Kirby, M. H., Kohli, J. M., Kozelov, A. V., Kraus, J., Kulikov, S., Kumar, A., Kupco, A., Kurča, T., Kuzmin, V. A., Kvita, J., Lammers, S., Landsberg, G., Lebrun, P., Lee, H. S., Lee, S. W., Lee, W. M., Lellouch, J., Li, L., Li, Q. Z., Lietti, S. M., Lim, J. K., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, Y., Liu, Z., Lobodenko, A., Lokajicek, M., de Sa, R. Lopes, Lubatti, H. J., Luna-Garcia, R., Lyon, A. L., Maciel, A. K. A., Mackin, D., Madar, R., Magaña-Villalba, R., Malik, S., Malyshev, V. L., Maravin, Y., Martínez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Miconi, F., Mondal, N. K., Muanza, G. S., Mulhearn, M., Nagy, E., Naimuddin, M., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Neustroev, P., Novaes, S. F., Nunnemann, T., Obrant, G., Orduna, J., Osman, N., Osta, J., Garzón, G. J. Otero y, Padilla, M., Pal, A., Parashar, N., Parihar, V., Park, S. K., Parsons, J., Partridge, R., Parua, N., Patwa, A., Penning, B., Perfilov, M., Peters, K., Peters, Y., Petridis, K., Petrillo, G., Pétroff, P., Piegaia, R., Piper, J., Pleier, M. -A., Podesta-Lerma, P. L. M., Podstavkov, V. M., Polozov, P., Popov, A. V., Prewitt, M., Price, D., Prokopenko, N., Protopopescu, S., Qian, J., Quadt, A., Quinn, B., Rangel, M. S., Ranjan, K., Ratoff, P. N., Razumov, I., Renkel, P., Rijssenbeek, M., Ripp-Baudot, I., Rizatdinova, F., Rominsky, M., Ross, A., Royon, C., Rubinov, P., Ruchti, R., Safronov, G., Sajot, G., Salcido, P., Sánchez-Hernández, A., Sanders, M. P., Sanghi, B., Santos, A. S., Savage, G., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schliephake, T., Schlobohm, S., Schwanenberger, C., Schwienhorst, R., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shchukin, A. A., Shivpuri, R. K., Simak, V., Sirotenko, V., Skubic, P., Slattery, P., Smirnov, D., Smith, K. J., Snow, G. R., Snow, J., Snyder, S., Söldner-Rembold, S., Sonnenschein, L., Soustruznik, K., Stark, J., Stolin, V., Stoyanova, D. A., Strauss, M., Strom, D., Stutte, L., Suter, L., Svoisky, P., Takahashi, M., Tanasijczuk, A., Taylor, W., Titov, M., Tokmenin, V. V., Tsai, Y. -T., Tsybychev, D., Tuchming, B., Tully, C., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Verdier, P., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vokac, P., Wahl, H. D., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weber, M., Welty-Rieger, L., White, A., Wicke, D., Williams, M. R. J., Wilson, G. W., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Xu, C., Yacoob, S., Yamada, R., Yang, W. -C., Yasuda, T., Yatsunenko, Y. A., Ye, Z., Yin, H., Yip, K., Youn, S. W., Yu, J., Zelitch, S., Zhao, T., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We measure the top quark mass (mt) in ppbar collisions at a center of mass energy of 1.96 TeV using dilepton ttbar->W+bW-bbar->l+nubl-nubarbbar events, where l denotes an electron, a muon, or a tau that decays leptonically. The data correspond to an integrated luminosity of 5.4 fb-1 collected with the D0 detector at the Fermilab Tevatron Collider. We obtain mt = 174.0 +- 1.8(stat) +- 2.4(syst) GeV, which is in agreement with the current world average mt = 173.3 +- 1.1 GeV. This is currently the most precise measurement of mt in the dilepton channel., Comment: 7 pages, 4 figures
Published: 2011
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34. He II 4686 in eta Carinae: collapse of the wind-wind collision region during periastron passage

Author: Teodoro, M., Damineli, A., Arias, J. I., de Araújo, F. X., Barbá, R. H., Corcoran, M. F., Fernandes, M. Borges, Fernández-Lajús, E., Fraga, L., Gamen, R. C., González, J. F., Groh, J. H., Marshall, J. L., McGregor, P. J., Morrell, N., Nicholls, D. C., Parkin, E. R., Pereira, C. B., Phillips, M. M., Solivella, G. R., Steiner, J. E., Stritzinger, M., Thompson, I., Torres, C. A. O., Torres, M. A. P., and Zevallos-Herencia, M. I.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The periodic spectroscopic events in eta Carinae are now well established and occur near the periastron passage of two massive stars in a very eccentric orbit. Several mechanisms have been proposed to explain the variations of different spectral features, such as an eclipse by the wind-wind collision boundary, a shell ejection from the primary star or accretion of its wind onto the secondary. All of them have problems explaining all the observed phenomena. To better understand the nature of the cyclic events, we performed a dense monitoring of eta Carinae with 5 Southern telescopes during the 2009 low excitation event, resulting in a set of data of unprecedented quality and sampling. The intrinsic luminosity of the He II 4686 emission line (L~310 Lsun) just before periastron reveals the presence of a very luminous transient source of extreme UV radiation emitted in the wind-wind collision (WWC) region. Clumps in the primary's wind probably explain the flare-like behavior of both the X-ray and He II 4686 light-curves. After a short-lived minimum, He II 4686 emission rises again to a ne, Comment: Two-column style; 18 pages, 10 figures, and 1 table. Accepted for publication in ApJ
Published: 2011
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35. Global X-ray properties of the O and B stars in Carina

Author: Naze, Y., Broos, P. S., Oskinova, L., Townsley, L. K., Cohen, D., Corcoran, M. F., Evans, N. R., Gagne, M., Moffat, A. F. J., Pittard, J. M., Rauw, G., ud-Doula, A., and Walborn, N. R.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The key empirical property of the X-ray emission from O stars is a strong correlation between the bolometric and X-ray luminosities. In the framework of the Chandra Carina Complex Project, 129 O and B stars have been detected as X-ray sources; 78 of those, all with spectral type earlier than B3, have enough counts for at least a rough X-ray spectral characterization. This leads to an estimate of the Lx/Lbol ratio for an exceptional number of 60 O stars belonging to the same region and triples the number of Carina massive stars studied spectroscopically in X-rays. The derived log(Lx/Lbol) is -7.26 for single objects, with a dispersion of only 0.21dex. Using the properties of hot massive stars listed in the literature, we compare the X-ray luminosities of different types of objects. In the case of O stars, the Lx/Lbol ratios are similar for bright and faint objects, as well as for stars of different luminosity classes or spectral types. Binaries appear only slightly harder and slightly more luminous in X-rays than single objects; the differences are not formally significant (at the 1% level), except for the Lx/Lbol ratio in the medium (1.0--2.5keV) energy band. Weak-wind objects have similar X-ray luminosities but they display slightly softer spectra compared to "normal" O stars with the same bolometric luminosity. Discarding three overluminous objects, we find a very shallow trend of harder emission in brighter objects. The properties of the few B stars bright enough to yield some spectral information appear to be different overall (constant X-ray luminosities, harder spectra), hinting that another mechanism for producing X-rays, besides wind shocks, might be at work. However, it must be stressed that the earliest and X-ray brightest amongst these few detected objects are similar to the latest O stars, suggesting a possibly smooth transition between the two processes., Comment: 30 pages, 9 figures. Accepted for the ApJS Special Issue on the Chandra Carina Complex Project (CCCP), scheduled for publication in May 2011. All 16 CCCP Special Issue papers are available at http://cochise.astro.psu.edu/Carina_public/special_issue.html through 2011 at least
Published: 2011
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36. The X-ray Lightcurve of WR 140

Author: Corcoran, M. F., Pollock, A. M. T., Hamaguchi, K., and Russell, C.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: WR 140 is a canonical massive "colliding wind" binary system in which periodically-varying X-ray emission is produced by the collision between the wind of the WC7 and O4-5 star components in the space between the two stars. We have obtained X-ray observations using the RXTE satellite observatory through almost one complete orbital cycle including two consecutive periastron passages. We discuss the results of this observing campaign, and the implications of the X-ray data for our understanding of the orbital dynamics and the stellar mass loss., Comment: 6 pages, 5 figures, Published in proceedings of "Stellar Winds in Interaction", editors T. Eversberg and J.H. Knapen. Full proceedings volume is available on http://www.stsci.de/pdf/arrabida.pdf
Published: 2011

37. The WR 140 periastron passage 2009: first results from MONS and other optical sources

Author: Fahed, R., Moffat, A. F. J., Zorec, J., Eversberg, T., Chené, A. N., Alves, F., Arnold, W., Bergmann, T., Carreira, L. F. Gouveia, Dias, F. Marques, Fernando, A., Gallego, J. Sanchez, Hunger, T., Knapen, J. H., Leadbeater, R., Morel, T., Rauw, G., Reinecke, N., Ribeiro, J., Romeo, N., Santos, E. M. dos, Schanne, L., Stahl, O., Stober, Ba., Stober, Be., Viegas, N. G. Correia, Vollmann, K., Corcoran, M. F., Dougherty, S. M., Pittard, J. M., Pollock, A. M. T., and Williams, P. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the results from the spectroscopic follow-up of WR140 (WC7 + O4-5) during its last periastron passage in January 2009. This object is known as the archetype of colliding wind binaries and has a relatively large period (~ 8 years) and eccentricity (~ 0.89). We provide updated values for the orbital parameters, new estimates for the WR and O star masses and new constraints on the mass-loss rates., Comment: 5 pages, 5 figures, Published in proceedings of "Stellar Winds in Interaction", editors T. Eversberg and J.H. Knapen. Full proceedings volume is available on http://www.stsci.de/pdf/arrabida.pdf
Published: 2011

38. Measurement of the W boson helicity in top quark decays using 5.4 fb^-1 of ppbar collision data

Author: Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Altona, A., Alverson, G., Alves, G. A., Ancu, L. S., Aoki, M., Arnoud, Y., Arov, M., Askew, A., Asman, B., Atramentov, O., Avila, C., BackusMayes, J., Badaud, F., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Barreto, J., Bartlett, J. F., Bassler, U., Bazterra, V., Beale, S., Bean, A., Begalli, M., Begel, M., Belanger-Champagne, C., Bellantoni, L., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besancon, M., Beuselinck, R., Bezzubov, V. A., Bhat, P. C., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Bolton, T. A., Boos, E. E., Borissov, G., Bose, T., Brandt, A., Brandt, O., Brock, R., Brooijmans, G., Bross, A., Brown, D., Brown, J., Bu, X. B., Buehler, M., Buescher, V., Bunichev, V., Burdinb, S., Burnett, T. H., Buszello, C. P., Calpas, B., Camacho-Perez, E., Carrasco-Lizarraga, M. A., Casey, B. C. K., Castilla-Valdez, H., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chen, G., Chevalier-Thery, S., Cho, D. K., Cho, S. W., Choi, S., Choudhary, B., Christoudias, T., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Croc, A., Cutts, D., Cwiok, M., Das, A., Davies, G., De, K., de Jong, S. J., De La Cruz-Burelo, E., Deliot, F., Demarteau, M., Demina, R., Denisov, D., Denisov, S. P., Desai, S., DeVaughan, K., Diehl, H. T., Diesburg, M., Dominguez, A., Dorland, T., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Edmunds, D., Ellison, J., Elvira, V. D., Enari, Y., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Ferbel, T., Fiedler, F., Filthaut, F., Fisher, W., Fisk, H. E., Fortner, M., Fox, H., Fuess, S., Gadfort, T., Garcia-Bellido, A., Gavrilov, V., Gay, P., Geist, W., Geng, W., Gerbaudo, D., Gerber, C. E., Gershtein, Y., Ginther, G., Golovanov, G., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Greenwood, Z. D., Gregores, E. M., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grunendahl, S., Grunewald, M. W., Guo, F., Gutierrez, G., Gutierrez, P., Haasc, A., Hagopian, S., Haley, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hohlfeld, M., Hossain, S., Hubacek, Z., Huske, N., Hynek, V., Iashvili, I., Illingworth, R., Ito, A. S., Jabeen, S., Jaffre, M., Jain, S., Jamin, D., Jesik, R., Johns, K., Johnson, M., Johnston, D., Jonckheere, A., Jonsson, P., Joshi, J., Juste, A., Kaadze, K., Kajfasz, E., Karmanov, D., Kasper, P. A., Katsanos, I., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Khatidze, D., Kirby, M. H., Kohli, J. M., Kozelov, A. V., Kraus, J., Kumar, A., Kupco, A., Kurca, T., Kuzmin, V. A., Kvita, J., Lammers, S., Landsberg, G., Lebrun, P., Lee, H. S., Lee, S. W., Lee, W. M., Lellouch, J., Li, L., Li, Q. Z., Lietti, S. M., Lim, J. K., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, Y., Liu, Z., Lobodenko, A., Lokajicek, M., Love, P., Lubatti, H. J., Luna-Garciae, R., Lyon, A. L., Maciel, A. K. A., Mackin, D., Madar, R., Magana-Villalba, R., Malik, S., Malyshev, V. L., Maravin, Y., Martinez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Mondal, N. K., Muanza, G. S., Mulhearn, M., Nagy, E., Naimuddin, M., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Neustroev, P., Novaes, S. F., Nunnemann, T., Obrant, G., Orduna, J., Osman, N., Osta, J., Garzon, G. J. Otero y, Owen, M., Padilla, M., Pangilinan, M., Parashar, N., Parihar, V., Park, S. K., Parsons, J., Partridge, R., Parua, N., Patwa, A., Penning, B., Perfilov, M., Peters, K., Peters, Y., Petrillo, G., Petroff, P., Piegaia, R., Piper, J., Pleier, M. -A., Podesta-Lerma, P. L. M., Podstavkov, V. M., Pol, M. -E., Polozov, P., Popov, A. V., Prewitt, M., Price, D., Protopopescu, S., Qian, J., Quadt, A., Quinn, B., Rangel, M. S., Ranjan, K., Ratoff, P. N., Razumov, I., Renkel, P., Rich, P., Rijssenbeek, M., Ripp-Baudot, I., Rizatdinova, F., Rominsky, M., Royon, C., Rubinov, P., Ruchti, R., Safronov, G., Sajot, G., Sanchez-Hernandez, A., Sanders, M. P., Sanghi, B., Santos, A. S., Savage, G., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schliephake, T., Schlobohm, S., Schwanenberger, C., Schwienhorst, R., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shchukin, A. A., Shivpuri, R. K., Simak, V., Sirotenko, V., Skubic, P., Slattery, P., Smirnov, D., Smith, K. J., Snow, G. R., Snow, J., Snyder, S., Soldner-Rembold, S., Sonnenschein, L., Sopczak, A., Sosebee, M., Soustruznik, K., Spurlock, B., Stark, J., Stolin, V., Stoyanova, D. A., Strauss, M., Strom, D., Stutte, L., Suter, L., Svoisky, P., Takahashi, M., Tanasijczuk, A., Taylor, W., Titov, M., Tokmenin, V. V., Tsai, Y. -T., Tsybychev, D., Tuchming, B., Tully, C., Tuts, P. M., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Verdier, P., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vint, P., Vokac, P., Wahl, H. D., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weberg, M., Welty-Rieger, L., White, A., Wicke, D., Williams, M. R. J., Wilson, G. W., Wimpenny, S. J., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Xu, C., Yacoob, S., Yamada, R., Yang, W. -C., Yasuda, T., Yatsunenko, Y. A., Ye, Z., Yin, H., Yip, K., Youn, S. W., Yu, J., Zelitch, S., Zhao, T., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We present a measurement of the helicity of the W boson produced in top quark decays using ttbar decays in the l+jets and dilepton final states selected from a sample of 5.4 fb^-1 of collisions recorded using the D0 detector at the Fermilab Tevatron ppbar collider. We measure the fractions of longitudinal and right-handed W bosons to be f_0 = 0.669 +- 0.102 [ +- 0.078 (stat.) +- 0.065 (syst.)] and f_+ = 0.023 +- 0.053 [+- 0.041 (stat.) +- 0.034 (syst.)], respectively. This result is consistent at the 98% level with the standard model. A measurement with f_0 fixed to the value from the standard model yields f_+ = 0.010 +- 0.037 [+- 0.022 (stat.) +- 0.030 (syst.) ]., Comment: To be submitted to Phys. Rev. D
Published: 2010
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39. Spiralling out of control: 3D hydrodynamical modelling of the colliding winds in $\eta\thinspace$Carinae

Author: Parkin, E. R., Pittard, J. M., Corcoran, M. F., and Hamaguchi, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Three dimensional (3D) adaptive-mesh refinement (AMR) hydrodynamical simulations of the wind-wind collision between the enigmatic super-massive star \etacar and its mysterious companion star are presented which include radiative driving of the stellar winds, gravity, optically-thin radiative cooling, and orbital motion. Simulations with static stars with a periastron passage separation reveal that the preshock companion star's wind speed is sufficiently reduced that radiative cooling in the postshock gas becomes important, permitting the runaway growth of non-linear thin shell (NTSI) instabilities which massively distort the WCR. However, large-scale simulations which include the orbital motion of the stars, show that orbital motion reduces the impact of radiative inhibition, and thus increases the acquired preshock velocities. As such, the postshock gas temperature and cooling time see a commensurate increase, and sufficient gas pressure is preserved to stabilize the WCR against catastrophic instability growth. We then compute synthetic X-ray spectra and lightcurves and find that, compared to previous models, the X-ray spectra agree much better with {\it XMM-Newton} observations just prior to periastron. The narrow width of the 2009 X-ray minimum can also be reproduced. However, the models fail to reproduce the extended X-ray mimimum from previous cycles. We conclude that the key to explaining the extended X-ray minimum is the rate of cooling of the companion star's postshock wind. If cooling is rapid then powerful NTSIs will heavily disrupt the WCR. Radiative inhibition of the companion star's preshock wind, albeit with a stronger radiation-wind coupling than explored in this work, could be an effective trigger., Comment: 25 pages, 20 figures, accepted for publication in ApJ
Published: 2010
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40. Precise Measurements of Direct CP Violation, CPT Symmetry, and Other Parameters in the Neutral Kaon System

Author: KTeV Collaboration, Abouzaid, E., Arenton, M., Barker, A. R., Barrio, M., Bellantoni, L., Blucher, E., Bock, G. J., Bown, C., Cheu, E., Coleman, R., Corcoran, M. D., Cox, B., Erwin, A. R., Escobar, C. O., Glazov, A., Golossanov, A., Gomes, R. A., Gouffon, P., Graham, J., Hamm, J., Hsiung, Y. B., Jensen, D. A., Kessler, R., Kotera, K., LaDue, J., Ledovskoy, A., McBride, P. L., Monnier, E., Nguyen, H., Niclasen, R., Phillips II, D. G., Prasad, V., Qi, X. R., Ramberg, E. J., Ray, R. E., Ronquest, M., Roodman, A., Santos, E., Shanahan, P., Shawhan, P. S., Slater, W., Smith, D., Solomey, N., Swallow, E. C., Taegar, S. A., Toale, P. A., Tschirhart, R., Wah, Y. W., Wang, J., White, H. B., Whitmore, J., Wilking, M. J., Winstein, B., Winston, R., Worcester, E. T., Yamanaka, T., Zimmerman, E. D., and Zukanovich, R. F.
Subjects: High Energy Physics - Experiment
Abstract: We present precise tests of CP and CPT symmetry based on the full dataset of K to pipi decays collected by the KTeV experiment at Fermi National Accelerator Laboratory during 1996, 1997, and 1999. This dataset contains 16 million K to 2pi0 and 69 million K to pi+pi- decays. We measure the direct CP violation parameter Re(epsilon'/epsilon) = (19.2 pm 2.1)x10-4. We find the KL-KS mass difference Deltam = (5270 pm 12)x10^6 hbar/s and the KS lifetime tauS = (89.62 pm 0.05)x10-12 s. We also measure several parameters that test CPT invariance. We find the difference between the phase of the indirect CP violation parameter, epsilon, and the superweak phase, phi_epsilon - phi_SW = (0.40 pm 0.56) degrees. We measure the difference of the relative phases between the CP violating and CP conserving decay amplitudes for K to pi+pi- (phi+-) and for K to 2pi0 (phi00), Delta phi = (0.30 pm 0.35) degrees. From these phase measurements, we place a limit on the mass difference between K0 and K0bar, DeltaM < 4.8 x 10-19 GeV/c^2 at 95% C.L. These results are consistent with those of other experiments, our own earlier measurements, and CPT symmetry., Comment: 28 pages, 30 figures; removed extra figure
Published: 2010
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41. Search for pair production of the scalar top quark in the electron-muon final state

Author: Abazov, V. M., Abbott, B., Abolins, M., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Altona, A., Alverson, G., Alves, G. A., Ancu, L. S., Aoki, M., Arnoud, Y., Arov, M., Askew, A., Åsman, B., Atramentov, O., Avila, C., BackusMayes, J., Badaud, F., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Barreto, J., Bartlett, J. F., Bassler, U., Bazterra, V., Beale, S., Bean, A., Begalli, M., Begel, M., Belanger-Champagne, C., Bellantoni, L., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besançon, M., Beuselinck, R., Bezzubov, V. A., Bhat, P. C., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Bolton, T. A., Boos, E. E., Borissov, G., Bose, T., Brandt, A., Brandt, O., Brock, R., Brooijmans, G., Bross, A., Brown, D., Brown, J., Bu, X. B., Buchholz, D., Buehler, M., Buescher, V., Bunichev, V., Burdinb, S., Burnett, T. H., Buszello, C. P., Calpas, B., Camacho-Pérez, E., Carrasco-Lizarraga, M. A., Casey, B. C. K., Castilla-Valdez, H., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chen, G., Chevalier-Théry, S., Cho, D. K., Cho, S. W., Choi, S., Choudhary, B., Christoudias, T., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Croc, A., Cutts, D., Ćwiok, M., Das, A., Davies, G., De, K., de Jong, S. J., De La Cruz-Burelo, E., Déliot, F., Demarteau, M., Demina, 47 R., Denisov, D., Denisov, S. P., Desai, S., DeVaughan, K., Diehl, H. T., Diesburg, M., Dominguez, A., Dorland, T., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Edmunds, D., Ellison, J., Elvira, V. D., Enari, Y., Eno, S., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Ferbel, T., Fiedler, F., Filthaut, F., Fisher, W., Fisk, H. E., Fortner, M., Fox, H., Fuess, S., Gadfort, T., Garcia-Bellido, A., Gavrilov, V., Gay, P., Geist, W., Geng, W., Gerbaudo, D., Gerber, C. E., Gershtein, Y., Ginther, G., Golovanov, G., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Greenwood, Z. D., Gregores, E. M., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grünendahl, S., Grünewald, M. W., Guo, F., Guo, J., Gutierrez, G., Gutierrez, P., Haasc, A., Hagopian, S., Haley, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hohlfeld, M., Hossain, S., Hubacek, Z., Huske, N., Hynek, V., Iashvili, I., Illingworth, R., Ito, A. S., Jabeen, S., Jaffré, M., Jain, S., Jamin, D., Jesik, R., Johns, K., Johnson, M., Johnston, D., Jonckheere, A., Jonsson, P., Joshi, J., Justed, A., Kaadze, K., Kajfasz, E., Karmanov, D., Kasper, P. A., Katsanos, I., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Khatidze, D., Kirby, M. H., Kohli, J. M., Kozelov, A. V., Kraus, J., Kumar, A., Kupco, A., Kurča, T., Kuzmin, V. A., Kvita, J., Lammers, S., Landsberg, G., Lebrun, P., Lee, H. S., Lee, S. W., Lee, W. M., Lellouch, J., Li, L., Li, Q. Z., Lietti, S. M., Lim, J. K., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, Y., Liu, Z., Lobodenko, A., Lokajicek, M., Love, P., Lubatti, H. J., Luna-Garciae, R., Lyon, A. L., Maciel, A. K. A., Mackin, D., Madar, R., Magaña-Villalba, R., Malik, S., Malyshev, V. L., Maravin, Y., Martínez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Mondal, N. K., Muanza, G. S., Mulhearn, M., Nagy, E., Naimuddin, M., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Neustroev, P., Novaes, S. F., Nunnemann, T., Obrant, G., Orduna, J., Osman, N., Osta, J., Garzón, G. J. Otero y, Owen, M., Padilla, M., Pangilinan, M., Parashar, N., Parihar, V., Park, S. K., Parsons, J., Partridgec, R., Parua, N., Patwa, A., Penning, B., Perfilov, M., Peters, K., Peters, Y., Petrillo, G., Pétroff, P., Piegaia, R., Piper, J., Pleier, M. -A., Podesta-Lermaf, P. L. M., Podstavkov, V. M., Pol, M. -E., Polozov, P., Popov, A. V., Prewitt, M., Price, D., Protopopescu, S., Qian, J., Quadt, A., Quinn, B., Rangel, M. S., Ranjan, K., Ratoff, P. N., Razumov, I., Renkel, P., Rich, P., Rijssenbeek, M., Ripp-Baudot, I., Rizatdinova, F., Rominsky, M., Royon, C., Rubinov, P., Ruchti, R., Safronov, G., Sajot, G., Sánchez-Hernández, A., Sanders, M. P., Sanghi, B., Santos, A. S., Savage, G., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schliephake, T., Schlobohm, S., Schwanenberger, C., Schwienhorst, R., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shchukin, A. A., Shivpuri, R. K., Simak, V., Sirotenko, V., Skubic, P., Slattery, P., Smirnov, D., Smith, K. J., Snow, G. R., Snow, J., Snyder, S., Söldner-Rembold, S., Sonnenschein, L., Sopczak, A., Sosebee, M., Soustruznik, K., Spurlock, B., Stark, J., Stolin, V., Stoyanova, D. A., Strauss, E., Strauss, M., Strom, D., Stutte, L., Svoisky, P., Takahashi, M., Tanasijczuk, A., Taylor, W., Titov, M., Tokmenin, V. V., Tsybychev, D., Tuchming, B., Tully, C., Tuts, P. M., Uvarov, L., Uzunyan, S. Uvarov S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Verdier, P., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vint, P., Vokac, P., Wahl, H. D., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weberg, M., Welty-Rieger, L., Wetstein, M., White, A., Williams, D. Wicke M. R. J., Wilson, G. W., Wimpenny, S. J., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Xu, C., Yacoob, S., Yamada, R., Yang, W. -C., Yasuda, T., Yatsunenko, Y. A., Ye, Z., Yin, H., Yip, K., Yoo, H. D., Youn, S. W., Yu, J., Zelitch, S., Zhao, T., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We report the result of a search for the pair production of the lightest supersymmetric partner of the top quark ($\tilde{t}_1$) in $p\bar{p}$ collisions at a center-of-mass energy of 1.96 TeV at the Fermilab Tevatron collider corresponding to an integrated luminosity of 5.4 fb$^{-1}$. The scalar top quarks are assumed to decay into a $b$ quark, a charged lepton, and a scalar neutrino ($\tilde{\nu}$), and the search is performed in the electron plus muon final state. No significant excess of events above the standard model prediction is detected, and improved exclusion limits at the 95% C.L. are set in the the ($M_{\tilde{t}_1}$,$M_{\tilde{\nu}}$) mass plane.
Published: 2010
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42. Determination of the width of the top quark

Author: Abazov, V. M., Abbott, B., Abolins, M., Acharya, B. S., Adams, M., Adams, T., Alexeev, G. D., Alkhazov, G., Altona, A., Alverson, G., Alves, G. A., Ancu, L. S., Aoki, M., Arnoud, Y., Arov, M., Askew, A., Åsman, B., Atramentov, O., Avila, C., BackusMayes, J., Badaud, F., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barberis, E., Baringer, P., Barreto, J., Bartlett, J. F., Bassler, U., Bazterra, V., Beale, S., Bean, A., Begalli, M., Begel, M., Belanger-Champagne, C., Bellantoni, L., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besançon, M., Beuselinck, R., Bezzubov, V. A., Bhat, P. C., Bhatnagar, V., Blazey, G., Blessing, S., Bloom, K., Boehnlein, A., Boline, D., Bolton, T. A., Boos, E. E., Borissov, G., Bose, T., Brandt, A., Brandt, O., Brock, R., Brooijmans, G., Bross, A., Brown, D., Brown, J., Bu, X. B., Buchholz, D., Buehler, M., Buescher, V., Bunichev, V., Burdinb, S., Burnett, T. H., Buszello, C. P., Calpas, B., Camacho-Pérez, E., Carrasco-Lizarraga, M. A., Casey, B. C. K., Castilla-Valdez, H., Chakrabarti, S., Chakraborty, D., Chan, K. M., Chandra, A., Chen, G., Chevalier-Théry, S., Cho, D. K., Cho, S. W., Choi, S., Choudhary, B., Christoudias, T., Cihangir, S., Claes, D., Clutter, J., Cooke, M., Cooper, W. E., Corcoran, M., Couderc, F., Cousinou, M. -C., Croc, A., Cutts, D., Ćwiok, M., Das, A., Davies, G., De, K., de Jong, S. J., De La Cruz-Burelo, E., Déliot, F., Demarteau, M., Demina, R., Denisov, D., Denisov, S. P., Desai, S., DeVaughan, K., Diehl, H. T., Diesburg, M., Dominguez, A., Dorland, T., Dubey, A., Dudko, L. V., Duggan, D., Duperrin, A., Dutt, S., Dyshkant, A., Eads, M., Edmunds, D., Ellison, J., Elvira, V. D., Enari, Y., Eno, S., Evans, H., Evdokimov, A., Evdokimov, V. N., Facini, G., Ferbel, T., Fiedler, F., Filthaut, F., Fisher, W., Fisk, H. E., Fortner, M., Fox, H., Fuess, S., Gadfort, T., Garcia-Bellido, A., Gavrilov, V., Gay, P., Geist, W., Geng, W., Gerbaudo, D., Gerber, C. E., Gershtein, Y., Ginther, G., Golovanov, G., Goussiou, A., Grannis, P. D., Greder, S., Greenlee, H., Greenwood, Z. D., Gregores, E. M., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grnendahl, S., Grünewald, M. W., Guo, F., Guo, J., Gutierrez, G., Gutierrez, P., Haasc, A., Hagopian, S., Haley, J., Han, L., Harder, K., Harel, A., Hauptman, J. M., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinson, A. P., Heintz, U., Hensel, C., La Cruz, I. Heredia-De, Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hoeneisen, B., Hohlfeld, M., Hossain, S., Hubacek, Z., Huske, N., Hynek, V., Iashvili, I., Illingworth, R., Ito, A. S., Jabeen, S., Jaffré, M., Jain, S., Jamin, D., Jesik, R., Johns, K., Johnson, M., Johnston, D., Jonckheere, A., Jonsson, P., Joshi, J., Justed, A., Kaadze, K., Kajfasz, E., Karmanov, D., Kasper, P. A., Katsanos, I., Kehoe, R., Kermiche, S., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Khatidze, D., Kirby, M. H., Kohli, J. M., Kozelov, A. V., Kraus, J., Kumar, A., Kupco, A., Kurča, T., Kuzmin, V. A., Kvita, J., Lammers, S., Landsberg, G., Lebrun, P., Lee, H. S., Lee, S. W., Lee, W. M., Lellouch, J., Li, L., Li, Q. Z., Lietti, S. M., Lim, J. K., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipton, R., Liu, Y., Liu, Z., Lobodenko, A., Lokajicek, M., Love, P., Lubatti, H. J., Luna-Garciae, R., Lyon, A. L., Maciel, A. K. A., Mackin, D., Madar, R., Magaña-Villalba, R., Malik, S., Malyshev, V. L., Maravin, Y., Martínez-Ortega, J., McCarthy, R., McGivern, C. L., Meijer, M. M., Melnitchouk, A., Menezes, D., Mercadante, P. G., Merkin, M., Meyer, A., Meyer, J., Mondal, N. K., Muanza, G. S., Mulhearn, M., Nagy, E., Naimuddin, M., Narain, M., Nayyar, R., Neal, H. A., Negret, J. P., Neustroev, P., Novaes, S. F., Nunnemann, T., Obrant, G., Orduna, J., Osman, N., Osta, J., Garzón, G. J. Otero y, Owen, M., Padilla, M., Pangilinan, M., Parashar, N., Parihar, V., Park, S. K., Parsons, J., Partridgec, R., Parua, N., Patwa, A., Penning, B., Perfilov, M., Peters, K., Peters, Y., Petrillo, G., Pétroff, P., Piegaia, R., Piper, J., Pleier, M. -A., Podesta-Lermaf, P. L. M., Podstavkov, V. M., Pol, M. -E., Polozov, P., Popov, A. V., Prewitt, M., Price, D., Protopopescu, S., Qian, J., Quadt, A., Quinn, B., Rangel, M. S., Ranjan, K., Ratoff, P. N., Razumov, I., Renkel, P., Rich, P., Rijssenbeek, M., Ripp-Baudot, I., Rizatdinova, F., Rominsky, M., Royon, C., Rubinov, P., Ruchti, R., Safronov, G., Sajot, G., Sánchez-Hernández, A., Sanders, M. P., Sanghi, B., Santos, A. S., Savage, G., Sawyer, L., Scanlon, T., Schamberger, R. D., Scheglov, Y., Schellman, H., Schliephake, T., Schlobohm, S., Schwanenberger, C., Schwienhorst, R., Sekaric, J., Severini, H., Shabalina, E., Shary, V., Shchukin, A. A., Shivpuri, R. K., Simak, V., Sirotenko, V., Skubic, P., Slattery, P., Smirnov, D., Smith, K. J., Snow, G. R., Snow, J., Snyder, S., Söldner-Rembold, S., Sonnenschein, L., Sopczak, A., Sosebee, M., Soustruznik, K., Spurlock, B., Stark, J., Stolin, V., Stoyanova, D. A., Strauss, E., Strauss, M., Strom, D., Stutte, L., Svoisky, P., Takahashi, M., Tanasijczuk, A., Taylor, W., Titov, M., Tokmenin, V. V., Tsybychev, D., Tuchming, B., Tully, C., Tuts, P. M., Uvarov, L., Uzunyan, S. Uvarov S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Verdier, P., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vilanova, D., Vint, P., Vokac, P., Wahl, H. D., Wang, M. H. L. S., Warchol, J., Watts, G., Wayne, M., Weberg, M., Welty-Rieger, L., Wetstein, M., White, A., Williams, D. Wicke M. R. J., Wilson, G. W., Wimpenny, S. J., Wobisch, M., Wood, D. R., Wyatt, T. R., Xie, Y., Xu, C., Yacoob, S., Yamada, R., Yang, W. -C., Yasuda, T., Yatsunenko, Y. A., Ye, Z., Yin, H., Yip, K., Yoo, H. D., Youn, S. W., Yu, J., Zelitch, S., Zhao, T., Zhou, B., Zhu, J., Zielinski, M., Zieminska, D., and Zivkovic, L.
Subjects: High Energy Physics - Experiment
Abstract: We extract the total width of the top quark, Gamma_t, from the partial decay width Gamma(t -> W b) measured using the t-channel cross section for single top quark production and from the branching fraction B(t -> W b) measured in ttbar events using up to 2.3 fb^-1 of integrated luminosity collected by the D0 Collaboration at the Tevatron ppbar Collider. The result is Gamma_t = 1.99 +0.69 -0.55 GeV, which translates to a top-quark lifetime of tau_t = (3.3 +1.3 -0.9) x 10^-25 s. Assuming a high mass fourth generation b' quark and unitarity of the four-generation quark-mixing matrix, we set the first upper limit on |Vtb'| < 0.63 at 95% C.L., Comment: submitted to Phys. Rev. Letters
Published: 2010
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43. Variability monitoring of OB stars during the Mons campaign

Author: Morel, T., Rauw, G., Eversberg, T., Alves, F., Arnold, W., Bergmann, T., Viegas, N. G. Correia, Fahed, R., Fernando, A., Carreira, L. F. Gouveia, Hunger, T., Knapen, J. H., Leadbeater, R., Dias, F. Marques, Moffat, A. F. J., Reinecke, N., Ribeiro, J., Romeo, N., Gallego, J. Sanchez, Santos, E. M. dos, Schanne, L., Stahl, O., Stober, Ba., Stober, Be., Vollmann, K., Corcoran, M. F., Dougherty, S. M., Hamaguchi, K., Pittard, J. M., Pollock, A. M. T., and Williams, P. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present preliminary results of a 3-month campaign carried out in the framework of the Mons project, where time-resolved Halpha observations are used to study the wind and circumstellar properties of a number of OB stars., Comment: 2 pages, 1 figure. To appear in proceedings of IAUS272 'Active OB Stars: Structure, Evolution, Mass Loss and Critical Limits'
Published: 2010
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44. Eta Carinae long-term variability

Author: Damineli, A., Teodoro, M., Corcoran, M., and Groh, J. H.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present preliminary results of our analysis on the long-term variations observed in the optical spectrum of the LBV star Eta Carinae. Based on the hydrogen line profiles, we conclude that the physical parameters of the primary star did not change in the last 15 years., Comment: 2 pages, 1 figure, IAUS 272 - Active OB Stars: Structure, Evolution, Mass Loss and Critical Limits
Published: 2010
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45. The D0 Silicon Microstrip Tracker

Author: Ahmed, S. N., Angstadt, R., Aoki, M., Åsman, B., Austin, S., Bagby, L., Barberis, E., Baringer, P., Bean, A., Bischoff, A., Blekman, F., Bolton, T. A., Boswell, C., Bowden, M., Browning, F., Buchholz, D., Burdin, S., Butler, D., Cease, H., Choi, S., Clark, A. R., Clutter, J., Cooper, A., Cooper, W. E., Corcoran, M., de Jong, S. J., Demarteau, M., Demina, R., Desai, S., Derylo, G., Ellison, J., Ermolov, P., Fagan, J., Fast, J., Filthaut, F., Foglesong, J., Fox, H., Galea, C. F., Gardner, J., Genik II, R. J., Gerber, C. E., Gershtein, Y., Gounder, K., Grinstein, S., Gu, W., Gutierrez, P., Haggerty, H., Hall, R. E., Hagopian, S., Hance, R., Harder, K., Heger, P., Heinson, A. P., Heintz, U., Hesketh, G., Hover, D., Howell, J., Hrycyk, M., Iashvili, I., Johnson, M., Jöstlein, H., Juste, A., Kahl, W., Kajfasz, E., Karmanov, D., Kesisoglou, S., Khanov, A., King, J., Kleinfelder, S., Kowalski, J., Krempetz, K., Kubantsev, M., Kulik, Y., Landsberg, G., Leflat, A., Lehner, F., Lipton, R., Mao, H. S., Martin, M., Mateski, J., Matulik, M., McKenna, M., Melnitchouk, A., Merkin, M., Mihalcea, D., Milgrome, O., Montgomery, H. E., Moua, S., Naumann, N. A., Nomerotski, A., Olis, D., O'Neil, D. C., Garzón, G. J. Otero y, Parua, N., Pawlak, J., Petteni, M., Quinn, B., Rapidis, P. A., Ratzmann, P., Rizatdinova, F., Roco, M., Rucinski, R., Rykalin, V., Schellman, H., Schmitt, W., Sellberg, G., Serritella, C., Shabalina, E., Sidwell, R. A., Simak, V., Smith, E., Squires, B., Stanton, N. R., Steinbrück, G., Strandberg, J., Strandberg, S., Strauss, M., Stredde, S., Toukhtarov, A., Tripathi, S. M., Trippe, T. G., Tsybychev, D., Utes, M., van Gemmeren, P., Vaz, M., Weber, M., Wijngaarden, D. A., Wish, J., Womersley, J., Yarema, R., Ye, Z., Zieminski, A., Zimmerman, T., and Zverev, E. G.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: This paper describes the mechanical design, the readout chain, the production, testing and the installation of the Silicon Microstrip Tracker of the D0 experiment at the Fermilab Tevatron collider. In addition, description of the performance of the detector during the experiment data collection between 2001 and 2010 is provided.
Published: 2010
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46. Understanding the X-ray Flaring from Eta Car

Author: Moffat, A. F. J. and Corcoran, M. F.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We quantify the rapid variations in X-ray brightness ("flares") from the extremely massive colliding wind binary Eta Carinae seen during the past three orbital cycles by RXTE. The observed flares tend to be shorter in duration and more frequent as periastron is approached, although the largest ones tend to be roughly constant in strength at all phases. Plausible scenarios include (1) the largest of multi-scale stochastic wind clumps from the LBV component entering and compressing the hard X-ray emitting wind-wind collision (WWC) zone, (2) large-scale corotating interacting regions in the LBV wind sweeping across the WWC zone, or (3) instabilities intrinsic to the WWC zone. The first one appears to be most consistent with the observations, requiring homologously expanding clumps as they propagate outward in the LBV wind and a turbulence-like power-law distribution of clumps, decreasing in number towards larger sizes, as seen in Wolf-Rayet winds., Comment: accepted by ApJ
Published: 2009
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47. Detection of Gamma-ray Emission from the Eta-Carinae Region

Author: Tavani, M., Sabatini, S., Pian, E., Bulgarelli, A., Caraveo, P., Viotti, R. F., Corcoran, M. F., Giuliani, A., Pittori, C., Verrecchia, F., Vercellone, S., Mereghetti, S., Argan, A., Barbiellini, G., Boffelli, F., Cattaneo, P. W., Chen, A. W., Cocco, V., D'Ammando, F., Costa, E., De Paris, G., Del Monte, E., Di Cocco, G., Donnarumma, I., Evangelista, Y., Ferrari, A., Feroci, M., Fiorini, M., Froysland, T., Fuschino, F., Galli, M., Gianotti, F., Labanti, C., Lapshov, I., Lazzarotto, F., Lipari, P., Longo, F., Marisaldi, M., Mastropietro, M., Morelli, E., Moretti, E., Morselli, A., Pacciani, L., Pellizzoni, A., Perotti, F., Piano, G., Picozza, P., Pilia, M., Porrovecchio, G., Pucella, G., Prest, M., Rapisarda, M., Rappoldi, A., Rubini, A., Soffitta, P., Trifoglio, M., Trois, A., Vallazza, E., Vittorini, V., Zambra, A., Zanello, D., Santolamazza, P., Giommi, P., Colafrancesco, S., Antonelli, L. A., and Salotti, L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results of extensive observations by the gamma-ray AGILE satellite of the Galactic region hosting the Carina nebula and the remarkable colliding wind binary Eta Carinae (Eta Car) during the period 2007 July to 2009 January. We detect a gamma-ray source (1AGL J1043-5931) consistent with the position of Eta Car. If 1AGL J1043-5931 is associated with the Eta Car system our data provide the long sought first detection above 100 MeV of a colliding wind binary. The average gamma-ray flux above 100 MeV and integrated over the pre-periastron period 2007 July to 2008 October is F = (37 +/- 5) x 10-8 ph cm-2 s-1 corresponding to an average gamma-ray luminosity of L = 3.4 x 10^34 erg s-1 for a distance of 2.3 kpc. We also report a 2-day gamma-ray flaring episode of 1AGL J1043-5931 on 2008 Oct. 11-13 possibly related to a transient acceleration and radiation episode of the strongly variable shock in the system., Comment: 5 pages, 4 figure, accepted for publication in ApJ Letters
Published: 2009
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48. 3D modelling of the colliding winds in Eta Carinae - evidence for radiative inhibition

Author: Parkin, E. R., Pittard, J. M., Corcoran, M. F., Hamaguchi, K., and Stevens, I. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The X-ray emission from the super-massive star Eta Carinae is simulated using a three dimensional model of the wind-wind collision. In the model the intrinsic X-ray emission is spatially extended and energy dependent. Absorption due to the unshocked stellar winds and the cooled postshock material from the primary LBV star is calculated as the intrinsic emission is ray-traced along multiple sightlines through the 3D spiral structure of the circumstellar environment. The observable emission is then compared to available X-ray data, including the lightcurve observed by the Rossi X-ray Timing Explorer (RXTE) and spectra observed by XMM-Newton. The orientation and eccentricity of the orbit are explored, as are the wind parameters of the stars and the nature and physics of their close approach. Our modelling supports a viewing angle with an inclination of ~ 42 degrees, consistent with the polar axis of the Homunculus nebula (Smith 2006), and the projection of the observer's line-of-sight onto the orbital plane has an angle of ~ 0 - 30 degrees in the prograde direction on the apastron side of the semi-major axis. However, there are significant discrepancies between the observed and model lightcurves and spectra through the X-ray minimum. In particular, the hard flux in our synthetic spectra is an order of magnitude greater than observed. Further calculations reveal that radiative inhibition significantly reduces the preshock velocity of the companion wind. As a consequence the hard X-ray emission is quenched, but it is unclear whether the long duration of the minimum is due solely to this mechanism alone. Models incorporating a collapse/disruption of the WCR and/or reduced preshock companion wind velocities bring the predicted emission and the observations into much better agreement (abridged)., Comment: 20 pages, 24 Figures, accepted to MNRAS
Published: 2009
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49. Modeling the RXTE light curve of $\eta$ Carinae from a 3-D SPH simulation of its binary wind collision

Author: Okazaki, A. T., Owocki, S. P., Russell, C. M., and Corcoran, M. F.
Subjects: Astrophysics
Abstract: The very massive star system $\eta$ Carinae exhibits regular 5.54-year (2024-day) period disruptive events in wavebands ranging from the radio to X-ray. There is a growing consensus that these events likely stem from periastron passage of an (as yet) unseen companion in a highly eccentric ($\epsilon \sim 0.9$) orbit. This paper presents three-dimensional (3-D) Smoothed Particle Hydrodynamics (SPH) simulations of the orbital variation of the binary wind-wind collision, and applies these to modeling the X-ray light curve observed by the Rossi X-ray Timing Explorer (RXTE). By providing a global 3-D model of the phase variation of the density of the interacting winds, the simulations allow computation of the associated variation in X-ray absorption, presumed here to originate from near the apex of the wind-wind interaction cone. We find that the observed RXTE light curve can be readily fit if the observer's line of sight is within this cone along the general direction of apastron. Specifically, the data are well fit by an assumed inclination $i = 45^{\circ}$ for the orbit's polar axis, which is thus consistent with orbital angular momentum being along the inferred polar axis of the Homunculus nebula. The fits also constrain the position angle $\phi$ that an orbital-plane projection makes with the apastron side of the semi-major axis, strongly excluding positions $\phi < 9^{\circ}$ along or to the retrograde side of the axis, with the best fit position given by $\phi = 27^{\circ}$. Overall the results demonstrate the utility of a fully 3-D dynamical model for constraining the geometric and physical properties of this complex colliding-wind binary system., Comment: 5 pages, 4 figures, accepted to MNRAS Letters
Published: 2008
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50. Final Results from the KTeV Experiment on the Decay KL -> pi0 gamma gamma

Author: KTeV Collaboration, Abouzaid, E., Arenton, M., Barker, A. R., Bellantoni, L., Blucher, E., Bock, G. J., Cheu, E., Coleman, R., Corcoran, M. D., Cox, B., Erwin, A. R., Escobar, C. O., Glazov, A., Golossanov, A., Gomes, R. A., Gouffon, P., Hsiung, Y. B., Jensen, D. A., Kessler, R., Kotera, K., Ledovskoy, A., McBride, P. L., Monnier, E., Nguyen, H., Niclasen, R., Phillips II, D. G., Ramberg, E. J., Ray, R. E., Ronquest, M., Santos, E., Slater, W., Smith, D., Solomey, N., Swallow, E. C., Toale, P. A., Tschirhart, R., Wah, Y. W., Wang, J., White, H. B., Whitmore, J., Wilking, M. J., Winstein, B., Winston, R., Worcester, E. T., Yamanaka, T., Zimmerman, E. D., and Zukanovich, R. F.
Subjects: High Energy Physics - Experiment
Abstract: We report on a new measurement of the branching ratio B(KL->pi0 gamma gamma)using the KTeV detector. We reconstruct 1982 events with an estimated background of 608, that results in B(KL -> pi0 gamma gamma) = (1.29 +/- 0.03(stat) +/- 0.05(syst)) x 10**-6. We also measure the parameter, aV, which characterizes the strength of vector meson exchange terms in this decay. We find aV = -0.31 +/- 0.05(stat) +/- 0.07(syst). These results utilize the full KTeV data set collected from 1997 to 2000 and supersede earlier KTeV measurements of the branching ratio and aV., Comment: 8 pages, 8 figures
Published: 2008
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