Author: "Williams, G. P." - Searchworks@Jio Institute Digital Library Search Results

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2,257 results on '"Williams, G. P."'

51. The electron-capture origin of supernova 2018zd

Author: Hiramatsu, Daichi, Howell, D. Andrew, Van Dyk, Schuyler D., Goldberg, Jared A., Maeda, Keiichi, Moriya, Takashi J., Tominaga, Nozomu, Nomoto, Ken’ichi, Hosseinzadeh, Griffin, Arcavi, Iair, McCully, Curtis, Burke, Jamison, Bostroem, K. Azalee, Valenti, Stefano, Dong, Yize, Brown, Peter J., Andrews, Jennifer E., Bilinski, Christopher, Williams, G. Grant, Smith, Paul S., Smith, Nathan, Sand, David J., Anand, Gagandeep S., Xu, Chengyuan, Filippenko, Alexei V., Bersten, Melina C., Folatelli, Gastón, Kelly, Patrick L., Noguchi, Toshihide, and Itagaki, Koichi
Published: 2021
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52. Spectropolarimetry of SN 2011dh in M51: geometric insights on a Type IIb supernova progenitor and explosion

Author: Mauerhan, Jon C., Williams, G. Grant, Leonard, Douglas C., Smith, Paul S., Filippenko, Alexei V., Smith, Nathan, Hoffman, Jennifer L., Huk, Leah, Clubb, Kelsey I., Silverman, Jeffrey M., Cenko, S. Bradley, Milne, Peter, Gal-Yam, Avishay, and Ben-Ami, Sagi
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present seven epochs of spectropolarimetry of the Type IIb supernova (SN) 2011dh in M51, spanning 86 days of its evolution. The first epoch was obtained 9 days after the explosion, when the photosphere was still in the depleted hydrogen layer of the stripped-envelope progenitor. Continuum polarization is securely detected at the level of P~0.5% through day 14 and appears to diminish by day 30, which is different from the prevailing trends suggested by studies of other core-collapse SNe. Time-variable modulations in P and position angle are detected across P-Cygni line features. H-alpha and HeI polarization peak after 30 days and exhibit position angles roughly aligned with the earlier continuum, while OI and CaII appear to be geometrically distinct. We discuss several possibilities to explain the evolution of the continuum and line polarization, including the potential effects of a tidally deformed progenitor star, aspherical radioactive heating by fast-rising plumes of Ni-56 from the core, oblique shock breakout, or scattering by circumstellar material. While these possibilities are plausible and guided by theoretical expectations, they are not unique solutions to the data. The construction of more detailed hydrodynamic and radiative-transfer models that incorporate complex aspherical geometries will be required to further elucidate the nature of the polarized radiation from SN 2011dh and other Type IIb supernovae., Comment: Post-proof edit. Accepted to MNRAS 2015 Aug 19
Published: 2015
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53. Scaling the Yield of Laser-Driven Electron-Positron Jets to Laboratory Astrophysical Applications

Author: Chen, Hui, Fiuza, F., Link, A., Hazi, A., Hill, M., Hoarty, D., James, S., Kerr, S., Meyerhofer, D. D., Myatt, J., Park, J., Sentoku, Y., and Williams, G. J.
Subjects: Physics - Plasma Physics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report new experimental results obtained on three different laser facilities that show directed laser-driven relativistic electron-positron jets with up to 30 times larger yields than previously obtained and a quadratic (~ E^2) dependence of the positron yield on the laser energy. This favorable scaling stems from a combination of higher energy electrons due to increased laser intensity and the recirculation of MeV electrons in the mm-thick target. Based on this scaling, first principles simulations predict the possibility of using such electron-positron jets, produced at upcoming high-energy laser facilities, to probe the physics of relativistic collisionless shocks in the laboratory., Comment: 10 pages, 3 figures. Accepted to be published on Physical Review Letters on April 23, 2015
Published: 2015
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54. Constraints on Type IIn Supernova Progenitor Outbursts from the Lick Observatory Supernova Search

Author: Bilinski, Christopher, Smith, Nathan, Li, Weidong, Williams, G. Grant, Zheng, WeiKang, and Filippenko, Alexei V.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We searched through roughly 12 years of archival survey data acquired by the Katzman Automatic Imaging Telescope (KAIT) as part of the Lick Observatory Supernova Search (LOSS) in order to detect or place limits on possible progenitor outbursts of Type IIn supernovae (SNe~IIn). The KAIT database contains multiple pre-SN images for 5 SNe~IIn (plus one ambiguous case of a SN IIn/imposter) within 50 Mpc. No progenitor outbursts are found using the false discovery rate (FDR) statistical method in any of our targets. Instead, we derive limiting magnitudes (LMs) at the locations of the SNe. These limiting magnitudes (typically reaching $m_R \approx 19.5\,\mathrm{mag}$) are compared to outbursts of SN 2009ip and $\eta$ Car, plus additional simulated outbursts. We find that the data for SN 1999el and SN 2003dv are of sufficient quality to rule out events $\sim40$ days before the main peak caused by initially faint SNe from blue supergiant (BSG) precursor stars, as in the cases of SN 2009ip and SN 2010mc. These SNe~IIn may thus have arisen from red supergiant progenitors, or they may have had a more rapid onset of circumstellar matter interaction. We also estimate the probability of detecting at least one outburst in our dataset to be $\gtrsim60\%$ for each type of the example outbursts, so the lack of any detections suggests that such outbursts are either typically less luminous (intrinsically or owing to dust) than $\sim -13\,\mathrm{mag}$, or not very common among SNe~IIn within a few years prior to explosion., Comment: 22 pages, 11 figures, deluxetable.sty used
Published: 2015
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55. PTF11iqb: Cool supergiant mass loss that bridges the gap between Type IIn and normal supernovae

Author: Smith, Nathan, Mauerhan, Jon C., Cenko, S. Bradley, Kasliwal, Mansi M., Silverman, Jeffrey M., Filippenko, Alexei V., Gal-Yam, Avishay, Clubb, Kelsey I., Graham, Melissa L., Leonard, Douglas C., Horst, J. Chuck, Williams, G. Grant, Andrews, Jennifer E., Kulkarni, Shrinivas R., Nugent, Peter, Sullivan, Mark, Maguire, Kate, Xu, Dong, and Ben-Ami, Sagi
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: PTF11iqb was initially classified as a TypeIIn event caught very early after explosion. It showed narrow Wolf-Rayet (WR) spectral features on day 2, but the narrow emission weakened quickly and the spectrum morphed to resemble those of Types II-L and II-P. At late times, Halpha emission exhibited a complex, multipeaked profile reminiscent of SN1998S. In terms of spectroscopic evolution, we find that PTF11iqb was a near twin of SN~1998S, although with weaker interaction with circumstellar material (CSM) at early times, and stronger CSM interaction at late times. We interpret the spectral changes as caused by early interaction with asymmetric CSM that is quickly (by day 20) enveloped by the expanding SN ejecta photosphere, but then revealed again after the end of the plateau when the photosphere recedes. The light curve can be matched with a simple model for weak CSM interaction added to the light curve of a normal SN~II-P. This plateau requires that the progenitor had an extended H envelope like a red supergiant, consistent with the slow progenitor wind speed indicated by narrow emission. The cool supergiant progenitor is significant because PTF11iqb showed WR features in its early spectrum --- meaning that the presence of such WR features in an early SN spectrum does not necessarily indicate a WR-like progenitor. [abridged] Overall, PTF11iqb bridges SNe~IIn with weaker pre-SN mass loss seen in SNe II-L and II-P, implying a continuum between these types., Comment: 21 pages, 12 figures, submitted to MNRAS
Published: 2015
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56. Evaluation of the Accuracy of a Video and AI Solution to Measure Lower Leg and Foot Volume

Author: Chausiaux O, Williams G, Nieznański M, Bagdu A, Downer P, Keyser M, and Husheer S
Subjects: ai, peripheral edema, congestion, medical device, heart failure, lymphedema, renal disease, Medical technology, R855-855.5
Abstract: Oriane Chausiaux,1 Gareth Williams,1 Michał Nieznański,1 Adem Bagdu,2 Philip Downer,1 Melanie Keyser,1 Shamus Husheer1 1Heartfelt Technologies Ltd, Cambridge, UK; 2Warwick Medical School, University of Warwick, Coventry, UKCorrespondence: Oriane Chausiaux Email oriane@hftech.orgBackground and Objectives: Peripheral edema, change in foot volume, is a marker of congestion which is regularly assessed in routine clinical care. A novel video and Artificial Intelligence (AI)-based solution used to measure anatomical parameters, including volume and foot length, Heartfelt HF-1, is compared to the laboratory gold standard (water displacement) and a medical disposable measuring tape.Design, Setting, Participants, and Measurements: 58 healthy volunteers were measured with the Heartfelt device; 22 were also measured with the water displacement method and 19 with the medical tape. Bland–Altman analysis was performed for both volumes and foot lengths. Left/right foot differences provided covariance-corrected standard error of measurement (ccSEM) and minimum detectable difference (MDD) for each measurement method.Results: Heartfelt device measured volumes displayed excellent correlation to the gold standard (water displacement), with Bland–Altman bias of +32mL ± 81mL (1 std.dev). Clinically important change in foot volume is approximately 13%. Water displacement yielded ccSEM of ± 32.1mL and MDD of 90mL (6.7% of average foot volume), while the Heartfelt device measurements yielded ccSEM of ± 12.6mL and MDD of 35.3mL (2.6% of average foot volume). The majority of differences were attributable to manual positioning of the patient foot in the waterbath.Conclusion: This study finds that in clinical and non-clinical settings, the Heartfelt device measures foot volume and length more precisely than either the water displacement technique or manual foot length measurements using a medical disposable tape, while having an excellent agreement with these methods.Keywords: AI, peripheral edema, congestion, -medical device, heart failure, lymphedema, renal disease
Published: 2021

57. Myosteatosis evaluation using erector spinae and psoas muscles to predict adverse events during adjuvant chemotherapy for breast cancer

Author: Aleixo, G. F. P., Yu, H., Chen, Y. T., Nyrop, K. A., Louie, R. J., Deal, A. M., Shachar, S. S., Muss, H. B., and Williams, G. R.
Published: 2021
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58. Between Republic and Empire : Interpretations of Augustus and His Principate

Author: Raaflaub, Kurt A., Toher, Mark, Bowersock, G. W., Eder, W., Galsterer, H., Gruen, E. S., Kellum, B. A., Linderski, J., Luce, T. J., Meier, C., Mierse, W., Nugent, S. G., Ostrow, S. E., Pollini, J., Putnam, M. C. J., Raaflaub, K. A., Samons, L. J., Reinhold, M., Swan, P. M., Stahl, H. P., Toher, M., Williams, G., Yavetz, Z., Raaflaub, Kurt A., Toher, Mark, Bowersock, G. W., Eder, W., Galsterer, H., Gruen, E. S., Kellum, B. A., Linderski, J., Luce, T. J., Meier, C., Mierse, W., Nugent, S. G., Ostrow, S. E., Pollini, J., Putnam, M. C. J., Raaflaub, K. A., Samons, L. J., Reinhold, M., Swan, P. M., Stahl, H. P., Toher, M., Williams, G., and Yavetz, Z.
Published: 2023
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59. Doping dependence of the upper critical field, superconducting current density and thermally activated flux flow activation energy in polycrystalline CeFeAsO1-xFx superconductors

Author: Chong, S. V., Williams, G. V. M., Sambale, S., and Kadowaki, K.
Subjects: Condensed Matter - Superconductivity
Abstract: We report the results from resistivity and magnetic measurements on polycrystalline Ce oxypnictide (CeFeAsO1-xFx) samples where x spans from 0.13 to 0.25. We find that the orbital limiting field is as high as 150 T and it systematically decreases with increasing doping. The Maki parameter is greater than one across the phase diagram and the large Maki parameter suggests that orbital and Pauli limiting effects contribute to the upper critical field. The broadening of the superconducting transition in the resistivity data was interpreted using the thermally activated flux flow (TAFF) model where we find that the TAFF activation energy, U0(B), is proportional to B^{-(gamma)} from 1 T to high fields, and (gamma) does not significantly change with doping. However, U0 and the superconducting critical current, Jc, are peaked in the mid-doping region (x = 0.15 to x = 0.20), and not in the low (x < 0.15) or high doping (x > 0.20) regions. Furthermore, U0 is correlated with Jc and follows the two fluid model for granular samples., Comment: 27 pages, 7 figures
Published: 2014
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60. Cassini ISS Mutual Event Astrometry of the Mid-sized Saturnian Satellites 2005-2012

Author: Cooper, N. J., Murray, C. D., Lainey, V., Tajeddine, R., Evans, M. W., and Williams, G. A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present astrometric observations of the Saturnian satellites Mimas, Enceladus, Tethys, Dione and Rhea from Cassini Imaging Science Subsystem (ISS) narrow-angle camera (NAC) images. Image sequences were designed to observe mutual occultations between these satellites. The positions of satellite centres were estimated by fitting ellipsoidal shape models to the measured limbs of the imaged satellites. Spacecraft pointing corrections were computed using the UCAC2 star catalogue. We provide a total of 2303 astrometric observations, resulting in 976 pairs, the remainder consisting of observations of a single satellite. Mean residuals for the individual satellite positions relative to the SAT360 ephemeris were 4.3 km in the line direction and -2.4 km in the sample direction, with standard deviations of 5.6 and 7.0 km respectively, an order of magnitude improvement in precision compared to published HST observations. By considering inter-satellite separations, uncertainties in camera pointing and spacecraft positioning along with possible biases in the individual positions of the satellites can be largely eliminated, resulting in an order-of-magnitude increase in accuracy compared to that achievable using the individual satellite positions. We show how factors relating to the viewing geometry cause small biases in the individual positions of order 0.28 pixel to become systematic across the dataset as a whole and discuss options for reducing their effects . The reduced astrometric data are provided in the form of individual positions for each satellite, together with the measured positions of reference stars, in order to allow more flexibility in the processing of the observations, taking into account possible future advances in limb-fitting techniques as well as the future availability of more accurate star catalogues, such as those from the GAIA mission., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2014
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61. The Physics of the B Factories

Author: Bevan, A. J., Golob, B., Mannel, Th., Prell, S., Yabsley, B. D., Abe, K., Aihara, H., Anulli, F., Arnaud, N., Aushev, T., Beneke, M., Beringer, J., Bianchi, F., Bigi, I. I., Bona, M., Brambilla, N., rodzicka, J. B, Chang, P., Charles, M. J., Cheng, C. H., Cheng, H. -Y., Chistov, R., Colangelo, P., Coleman, J. P., Drutskoy, A., Druzhinin, V. P., Eidelman, S., Eigen, G., Eisner, A. M., Faccini, R., Flood, K. T ., Gambino, P., Gaz, A., Gradl, W., Hayashii, H., Higuchi, T., Hulsbergen, W. D., Hurth, T., Iijima, T., Itoh, R., Jackson, P. D., Kass, R., Kolomensky, Yu. G., Kou, E., Križan, P., Kronfeld, A., Kumano, S., Kwon, Y. J., Latham, T. E., Leith, D. W. G. S., Lüth, V., Martinez-Vidal, F., Meadows, B. T., Mussa, R., Nakao, M., Nishida, S., Ocariz, J., Olsen, S. L., Pakhlov, P., Pakhlova, G., Palano, A., Pich, A., Playfer, S., Poluektov, A., Porter, F. C., Robertson, S. H., Roney, J. M., Roodman, A., Sakai, Y., Schwanda, C., Schwartz, A. J., Seidl, R., Sekula, S. J., Steinhauser, M., Sumisawa, K., Swanson, E. S., Tackmann, F., Trabelsi, K., Uehara, S., Uno, S., van der Water, R., Vasseur, G., Verkerke, W., Waldi, R., Wang, M. Z., Wilson, F. F., Zupan, J., Zupanc, A., Adachi, I., Albert, J., Banerjee, Sw., Bellis, M., Ben-Haim, E., Biassoni, P., Cahn, R. N., Cartaro, C., Chauveau, J., Chen, C., Chiang, C. C., Cowan, R., Dalseno, J., Davier, M., Davies, C., Dingfelder, J. C., nard, B. Eche, Epifanov, D., Fulsom, B. G., Gabareen, A. M., Gary, J. W., Godang, R., Graham, M. T., Hafner, A., Hamilton, B., Hartmann, T., Hayasaka, K., Hearty, C., Iwasaki, Y., Khodjamirian, A., Kusaka, A., Kuzmin, A., Lafferty, G. D., Lazzaro, A., Li, J., Lindemann, D., Long, O., Lusiani, A., Marchiori, G., Martinelli, M., Miyabayashi, K., Mizuk, R., Mohanty, G. B., Muller, D. R., Nakazawa, H., Ongmongkolkul, P., Pacetti, S., Palombo, F., Pedlar, T. K., Piilonen, L. E., Pilloni, A., Poireau, V., Prothmann, K., Pulliam, T., Rama, M., Ratcliff, B. N., Roudeau, P., Schrenk, S., Schroeder, T., Schubert, K. R., Shen, C. P., Shwartz, B., Soffer, A., Solodov, E. P., Somov, A., Starič, M., Stracka, S., Telnov, A. V., Todyshev, K. Yu., Tsuboyama, T., Uglov, T., Vinokurova, A., Walsh, J. J., Watanabe, Y., Won, E., Wormser, G., Wright, D. H., Ye, S., Zhang, C. C., Abachi, S., Abashian, A., Abe, N., Abe, R., Abe, T., Abrams, G. S., Adam, I., Adamczyk, K., Adametz, A., Adye, T., Agarwal, A., Ahmed, H., Ahmed, M., Ahmed, S., Ahn, B. S., Ahn, H. S., Aitchison, I. J. R., Akai, K., Akar, S., Akatsu, M., Akemoto, M., Akhmetshin, R., Akre, R., Alam, M. S., Albert, J. N., Aleksan, R., Alexander, J. P., Alimonti, G., Allen, M. T., Allison, J., Allmendinger, T., Alsmiller, J. R. G., Altenburg, D., Alwyn, K. E., An, Q., Anderson, J., Andreassen, R., Andreotti, D., Andreotti, M., Andress, J. C., Angelini, C., Anipko, D., Anjomshoaa, A., Anthony, P. L., Antillon, E. A., Antonioli, E., Aoki, K., Arguin, J. F., Arinstein, K., Arisaka, K., Asai, K., Asai, M., Asano, Y., Asgeirsson, D. J., Asner, D. M., Aso, T., Aspinwall, M. L., Aston, D., Atmacan, H., Aubert, B., Aulchenko, V., Ayad, R., Azemoon, T., Aziz, T., Azzolini, V., Azzopardi, D. E., Baak, M. A., Back, J. J., Bagnasco, S., Bahinipati, S., Bailey, D. S., Bailey, S., Bailly, P., van Bakel, N., Bakich, A. M., Bala, A., Balagura, V., Baldini-Ferroli, R., Ban, Y., Banas, E., Band, H. R., Banerjee, S., Baracchini, E., Barate, R., Barberio, E., Barbero, M., Bard, D. J., Barillari, T., Barlow, N. R., Barlow, R. J., Barrett, M., Bartel, W., Bartelt, J., Bartoldus, R., Batignani, G., Battaglia, M., Bauer, J. M., Bay, A., Beaulieu, M., Bechtle, P., Beck, T. W., Becker, J., Becla, J., Bedny, I., Behari, S., Behera, P. K., Behn, E., Behr, L., Beigbeder, C., Beiline, D., Bell, R., Bellini, F., Bellodi, G., Belous, K., Benayoun, M., Benelli, G., Benitez, J. F., Benkebil, M., Berger, N., Bernabeu, J., Bernard, D., Bernet, R., Bernlochner, F. U., Berryhill, J. W., Bertsche, K., Besson, P., Best, D. S., Bettarini, S., Bettoni, D., Bhardwaj, V., Bhimji, W., Bhuyan, B., Biagini, M. E., Biasini, M., van Bibber, K., Biesiada, J., Bingham, I., Bionta, R. M., Bischofberger, M., Bitenc, U., Bizjak, I., Blanc, F., Blaylock, G., Blinov, V. E., Bloom, E., Bloom, P. C., Blount, N. L., Blouw, J., Bly, M., Blyth, S., Boeheim, C. T., Bomben, M., Bondar, A., Bondioli, M., Bonneaud, G. R., Bonvicini, G., Booke, M., Booth, J., Borean, C., Borgland, A. W., Borsato, E., Bosi, F., Bosisio, L., Botov, A. A., Bougher, J., Bouldin, K., Bourgeois, P., Boutigny, D., Bowerman, D. A., Boyarski, A. M., Boyce, R. F., Boyd, J. T., Bozek, A., Bozzi, C., Bračko, M., Brandenburg, G., Brandt, T., Brau, B., Brau, J., Breon, A. B., Breton, D., Brew, C., Briand, H., Bright-Thomas, P. G., Brigljević, V., Britton, D. I., Brochard, F., Broomer, B., Brose, J., Browder, T. E., Brown, C. L., Brown, C. M., Brown, D. N., Browne, M., Bruinsma, M., Brunet, S., Bucci, F., Buchanan, C., Buchmueller, O. L., Bünger, C., Bugg, W., Bukin, A. D., Bula, R., Bulten, H., Burchat, P. R., Burgess, W., Burke, J. P., Button-Shafer, J., Buzykaev, A. R., Buzzo, A., Cai, Y., Calabrese, R., Calcaterra, A., Calderini, G., Camanzi, B., Campagna, E., Campagnari, C., Capra, R., Carassiti, V., Carpinelli, M., Carroll, M., Casarosa, G., Casey, B. C. K., Cason, N. M., Castelli, G., Cavallo, N., Cavoto, G., Cecchi, A., Cenci, R., Cerizza, G., Cervelli, A., Ceseracciu, A., Chai, X., Chaisanguanthum, K. S., Chang, M. C., Chang, Y. H., Chang, Y. W., Chao, D. S., Chao, M., Chao, Y., Charles, E., Chavez, C. A., Cheaib, R., Chekelian, V., Chen, A., Chen, E., Chen, G. P., Chen, H. F., Chen, J. -H., Chen, J. C., Chen, K. F., Chen, P., Chen, S., Chen, W. T., Chen, X., Chen, X. R., Chen, Y. Q., Cheng, B., Cheon, B. G., Chevalier, N., Chia, Y. M., Chidzik, S., Chilikin, K., Chistiakova, M. V., Cizeron, R., Cho, I. S., Cho, K., Chobanova, V., Choi, H. H. F., Choi, K. S., Choi, S. K., Choi, Y., Choi, Y. K., Christ, S., Chu, P. H., Chun, S., Chuvikov, A., Cibinetto, G., Cinabro, D., Clark, A. R., Clark, P. J., Clarke, C. K., Claus, R., Claxton, B., Clifton, Z. C., Cochran, J., Cohen-Tanugi, J., Cohn, H., Colberg, T., Cole, S., Colecchia, F., Condurache, C., Contri, R., Convert, P., Convery, M. R., Cooke, P., Copty, N., Cormack, C. M., Corso, F. Dal, Corwin, L. A., Cossutti, F., Cote, D., Ramusino, A. Cotta, Cottingham, W. N., Couderc, F., Coupal, D. P., Covarelli, R., Cowan, G., Craddock, W. W., Crane, G., Crawley, H. B., Cremaldi, L., Crescente, A., Cristinziani, M., Crnkovic, J., Crosetti, G., Cuhadar-Donszelmann, T., Cunha, A., Curry, S., D'Orazio, A., Dû, S., Dahlinger, G., Dahmes, B., Dallapiccola, C., Danielson, N., Danilov, M., Das, A., Dash, M., Dasu, S., Datta, M., Daudo, F., Dauncey, P. D., David, P., Davis, C. L., Day, C. T., De Mori, F., De Domenico, G., De Groot, N., De la Vaissière, C., de la Vaissière, Ch., de Lesquen, A., De Nardo, G., de Sangro, R., De Silva, A., DeBarger, S., Decker, F. J., Sanchez, P. del Amo, Del Buono, L., Del Gamba, V., del Re, D., Della Ricca, G., Denig, A. G., Derkach, D., Derrington, I. M., DeStaebler, H., Destree, J., Devmal, S., Dey, B., Di Girolamo, B., Di Marco, E., Dickopp, M., Dima, M. O., Dittrich, S., Dittongo, S., Dixon, P., Dneprovsky, L., Dohou, F., Doi, Y., Doležal, Z., Doll, D. A., Donald, M., Dong, L., Dong, L. Y., Dorfan, J., Dorigo, A., Dorsten, M. P., Dowd, R., Dowdell, J., Drásal, Z., Dragic, J., Drummond, B. W., Dubitzky, R. S., Dubois-Felsmann, G. P., Dubrovin, M. S., Duh, Y. C., Duh, Y. T., Dujmic, D., Dungel, W., Dunwoodie, W., Dutta, D., Dvoretskii, A., Dyce, N., Ebert, M., Eckhart, E. A., Ecklund, S., Eckmann, R., Eckstein, P., Edgar, C. L., Edwards, A. J., Egede, U., Eichenbaum, A. M., Elmer, P., Emery, S., Enari, Y., Enomoto, R., Erdos, E., Erickson, R., Ernst, J. A., Erwin, R. J., Escalier, M., Eschenburg, V., Eschrich, I., Esen, S., Esteve, L., Evangelisti, F., Everton, C. W., Eyges, V., Fabby, C., Fabozzi, F., Fahey, S., Falbo, M., Fan, S., Fang, F., Fanin, C., Farbin, A., Farhat, H., Fast, J. E., Feindt, M., Fella, A., Feltresi, E., Ferber, T., Fernholz, R. E., Ferrag, S., Ferrarotto, F., Ferroni, F., Field, R. C., Filippi, A., Finocchiaro, G., Fioravanti, E., da Costa, J. Firmino, Fischer, P. -A., Fisher, A., Fisher, P. H., Flacco, C. J., Flack, R. L., Flaecher, H. U., Flanagan, J., Flanigan, J. M., Ford, K. E., Ford, W. T., Forster, I. J., Forti, A. C., Forti, F., Fortin, D., Foster, B., Foulkes, S. D., Fouque, G., Fox, J., Franchini, P., Sevilla, M. Franco, Franek, B., Frank, E. D., Fransham, K. B., Fratina, S., Fratini, K., Frey, A., Frey, R., Friedl, M., Fritsch, M., Fry, J. R., Fujii, H., Fujikawa, M., Fujita, Y., Fujiyama, Y., Fukunaga, C., Fukushima, M., Fullwood, J., Funahashi, Y., Funakoshi, Y., Furano, F., Furman, M., Furukawa, K., Futterschneider, H., Gabathuler, E., Gabriel, T. A., Gabyshev, N., Gaede, F., Gagliardi, N., Gaidot, A., Gaillard, J. -M., Gaillard, J. R., Galagedera, S., Galeazzi, F., Gallo, F., Gamba, D., Gamet, R., Gan, K. K., Gandini, P., Ganguly, S., Ganzhur, S. F., Gao, Y. Y., Gaponenko, I., Garmash, A., Tico, J. Garra, Garzia, I., Gaspero, M., Gastaldi, F., Gatto, C., Gaur, V., Geddes, N. I., Geld, T. L., Genat, J. -F., George, K. A., George, M., George, S., Georgette, Z., Gershon, T. J., Gill, M. S., Gillard, R., Gilman, J. D., Giordano, F., Giorgi, M. A., Giraud, P. -F., Gladney, L., Glanzman, T., Glattauer, R., Go, A., Goetzen, K., Goh, Y. M., Gokhroo, G., Goldenzweig, P., Golubev, V. B., Gopal, G. P., Gordon, A., Gorišek, A., Goriletsky, V. I., Gorodeisky, R., Gosset, L., Gotow, K., Gowdy, S. 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P., Treadwell, E., Triggiani, G., Trincaz-Duvoid, S., Trischuk, W., Troost, D., Trunov, A., Tsai, K. L., Tsai, Y. T., Tsujita, Y., Tsukada, K., Tsukamoto, T., Tuggle, J. M., Tumanov, A., Tung, Y. W., Turnbull, L., Turner, J., Turri, M., Uchida, K., Uchida, M., Uchida, Y., Ueki, M., Ueno, K., Ujiie, N., Ulmer, K. A., Unno, Y., Urquijo, P., Ushiroda, Y., Usov, Y., Usseglio, M., Usuki, Y., Uwer, U., Va'vra, J., Vahsen, S. E., Vaitsas, G., Valassi, A., Vallazza, E., Vallereau, A., Vanhoefer, P., van Hoek, W. C., Van Hulse, C., van Winkle, D., Varner, G., Varnes, E. W., Varvell, K. E., Vasileiadis, G., Velikzhanin, Y. S., Verderi, M., Versillé, S., Vervink, K., Viaud, B., Vidal, P. B., Villa, S., Villanueva-Perez, P., Vinograd, E. L., Vitale, L., Vitug, G. M., Voß, C., Voci, C., Voena, C., Volk, A., von Wimmersperg-Toeller, J. H., Vorobyev, V., Vossen, A., Vuagnin, G., Vuosalo, C. O., Wacker, K., Wagner, A. P., Wagner, D. L., Wagner, G., Wagner, M. N., Wagner, S. R., Wagoner, D. E., Walker, D., Walkowiak, W., Wallom, D., Wang, C. C., Wang, C. H., Wang, J., Wang, J. G., Wang, K., Wang, L., Wang, L. L., Wang, P., Wang, T. J., Wang, W. F., Wang, X. L., Wang, Y. F., Wappler, F. R., Watanabe, M., Watson, A. T., Watson, J. E., Watson, N. K., Watt, M., Weatherall, J. H., Weaver, M., Weber, T., Wedd, R., Wei, J. T., Weidemann, A. W., Weinstein, A. J. R., Wenzel, W. A., West, C. A., West, C. G., West, T. J., White, E., White, R. M., Wicht, J., Widhalm, L., Wiechczynski, J., Wienands, U., Wilden, L., Wilder, M., Williams, D. C., Williams, G., Williams, J. C., Williams, K. M., Williams, M. I., Willocq, S. Y., Wilson, J. R., Wilson, M. G., Wilson, R. J., Winklmeier, F., Winstrom, L. O., Winter, M. A., Wisniewski, W. J., Wittgen, M., Wittlin, J., Wittmer, W., Wixted, R., Woch, A., Wogsland, B. J., Wong, Q. K., Wray, B. C., Wren, A. C., Wright, D. M., Wu, C. H., Wu, J., Wu, S. L., Wulsin, H. W., Xella, S. M., Xie, Q. L., Xie, Y., Xu, Z. Z., Yèche, Ch., Yamada, Y., Yamaga, M., Yamaguchi, A., Yamaguchi, H., Yamaki, T., Yamamoto, H., Yamamoto, N., Yamamoto, R. K., Yamamoto, S., Yamanaka, T., Yamaoka, H., Yamaoka, J., Yamaoka, Y., Yamashita, Y., Yamauchi, M., Yan, D. S., Yan, Y., Yanai, H., Yanaka, S., Yang, H., Yang, R., Yang, S., Yarritu, A. K., Yashchenko, S., Yashima, J., Yasin, Z., Yasu, Y., Ye, S. W., Yeh, P., Yi, J. I., Yi, K., Yi, M., Yin, Z. W., Ying, J., Yocky, G., Yokoyama, K., Yokoyama, M., Yokoyama, T., Yoshida, K., Yoshida, M., Yoshimura, Y., Young, C. C., Yu, C. X., Yu, Z., Yuan, C. Z., Yuan, Y., Yumiceva, F. X., Yusa, Y., Yushkov, A. N., Yuta, H., Zacek, V., Zain, S. B., Zallo, A., Zambito, S., Zander, D., Zang, S. L., Zanin, D., Zaslavsky, B. G., Zeng, Q. L., Zghiche, A., Zhang, B., Zhang, J., Zhang, L., Zhang, L. M., Zhang, S. Q., Zhang, Z. P., Zhao, H. W., Zhao, M., Zhao, Z. G., Zheng, Y., Zheng, Y. H., Zheng, Z. P., Zhilich, V., Zhou, P., Zhu, R. Y., Zhu, Y. S., Zhu, Z. M., Zhulanov, V., Ziegler, T., Ziegler, V., Zioulas, G., Zisman, M., Zito, M., Zürcher, D., Zwahlen, N., Zyukova, O., Živko, T., and Žontar, D.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: This work is on the Physics of the B Factories. Part A of this book contains a brief description of the SLAC and KEK B Factories as well as their detectors, BaBar and Belle, and data taking related issues. Part B discusses tools and methods used by the experiments in order to obtain results. The results themselves can be found in Part C. Please note that version 3 on the archive is the auxiliary version of the Physics of the B Factories book. This uses the notation alpha, beta, gamma for the angles of the Unitarity Triangle. The nominal version uses the notation phi_1, phi_2 and phi_3. Please cite this work as Eur. Phys. J. C74 (2014) 3026., Comment: 928 pages, version 3 (arXiv:1406.6311v3) corresponds to the alpha, beta, gamma version of the book, the other versions use the phi1, phi2, phi3 notation
Published: 2014
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62. Multi-epoch spectropolarimetry of SN 2009ip: direct evidence for aspherical circumstellar material

Author: Mauerhan, Jon C., Williams, G. Grant, Smith, Nathan, Smith, Paul S., Filippenko, Alexei V., Hoffman, Jennifer L., Leonard, Douglas C., Milne, Peter, Clubb, Kelsey I., Fox, Ori D., and Kelly, Patrick L.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present spectropolarimetry of SN 2009ip throughout the evolution of its 2012 explosion. During the initial 2012a phase, when the source spectrum exhibits broad P-Cygni lines, we measure a V-band polarization of P~0.9% at a position angle of ~166 deg, indicating substantial asphericity for the 2012a outflow. Near the subsequent peak of the 2012b phase, when the spectrum shows signs of intense interaction with circumstellar material (CSM), we measure P~1.7% at a position angle of 72 deg, indicating a separate physical component of polarization, which has a higher degree of asphericity than the 2012a outflow and an orthogonal axis of symmetry on the sky. Around 30 days past peak, which is coincident with a bump in the declining light curve, we measure P~0.7% and significant variations in P across some broad lines, particularly HeI/NaI. By 60 days past peak the source appears to be approaching a low value of interstellar polarization (P<0.2%). The results are consistent with a scenario in which a potentially bipolar explosion during 2012a impacts a toroidal distribution of CSM, thereby causing the 2012b brightening. Orthogonality between the 2012a and 2012b geometries is inconsistent with the hypothesis that the 2012a event launched the CSM that was hit 40 days later by material from the 2012b event. Rather, the aspherical CSM probably has a separate origin associated with the outbursts of the stellar progenitor during prior years. Previous calculations that assumed spherical symmetry for the CSM have underestimated the required explosion energy, as the results suggest that <10% of the fast SN ejecta participated in strong CSM interaction during the 2012b phase. In light of the spectropolarimetric results, a kinetic energy of 1e51 erg for the ejecta is difficult to avoid, supporting the interpretation that the 2012 outburst was the result of a core-collapse supernova explosion (abridged), Comment: Accepted to MNRAS 2014 Apr 7. Accepted version. 15 pages, 10 figures
Published: 2014
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63. TB and HIV Epidemiology and Collaborative Service: Evidence from Ethiopia, 2011–2015

Author: Gelaw YA, Assefa Y, Soares Magalhaes RJ, Demissie M, Tadele W, Dhewantara PW, and Williams G
Subjects: tuberculosis (tb), hiv, collaborative-services, implementations, ethiopia, Immunologic diseases. Allergy, RC581-607
Abstract: Yalemzewod Assefa Gelaw,1,2 Yibeltal Assefa,2 Ricardo J Soares Magalhaes,3,4 Minilik Demissie,5 Wegayehu Tadele,5 Pandji Wibawa Dhewantara,3,6 Gail Williams2 1Institute of Public Health, College of Medicine and Health Science, University of Gondar, Gondar 196, Ethiopia; 2School of Public Health, Faculty of Medicine, The University of Queensland, Brisbane, Queensland 4006, Australia; 3UQ Spatial Epidemiology Laboratory, School of Veterinary Science, Faculty of Science, the University of Queensland, Gatton 4343, Queensland, Australia; 4Children’s Health and Environment Program, Child Health Research Centre, Faculty of Medicine, The University of Queensland, Brisbane 4101, Queensland, Australia; 5HIV/AIDS and Tuberculosis Research Directorate, Ethiopian Public Health Institute (EPHI), Addis Ababa, Ethiopia; 6Pangandaran Unit for Health Research and Development, National Institute of Health Research and Development, Ministry of Health of Indonesia, Pangandaran 46396, West Java, IndonesiaCorrespondence: Yalemzewod Assefa GelawSchool of Public Health, Faculty of Medicine, The University of Queensland, 288 Herston Road, Herston, Brisbane, Queensland 4006, AustraliaTel +61-469738918Email yalassefa@gmail.comBackground: Integrating and scaling up tuberculosis (TB) and HIV services are essential strategies to achieve the combined goals ending both TB and HIV, especially in TB and HIV high burden countries. This study aimed to examine the prevalence of TB and HIV co-infection and the implementation of collaborative services in Ethiopia.Methods: We used a national sentinel surveillance TB/HIV co-infection collected between 2010 and 2015. The Ethiopian Public Health Institute collected and collated the data quarterly from 79 health facilities in nine regional states and two city administrations.Results: A total of 55,336 people living with HIV/AIDS were screened for active TB between 2011 and 2015. Of these, 7.3% were found co-infected with TB, and 13% TB-negative PLWHA were on isoniazid preventive therapy. Nine out of ten (89.2%) active TB patients were screened for HIV counselling and 17.8% were found to be HIV positive; 78.2% and 53.0% of HIV/TB co-infected patients were receiving cotrimoxazole preventive therapy and antiretroviral treatment, respectively.Conclusion: This study showed that the prevalence of TB and HIV co-infection failed to decrease over the study period, and that, while there was an increasing trend for integration of collaborative services, this was not uniform over time. Aligning and integrating TB and HIV responses are still needed to achieve the target of ending TB and HIV by 2030.Keywords: tuberculosis, TB, HIV, collaborative services, implementations, Ethiopia
Published: 2020

64. Self-Perceived Confidence of Medical Students Communicating with Pediatric Patients in a 7-Week Pediatric Placement: A Pilot Survey

Author: Teh JJ, Cheung KY, Patrick Y, Panahi M, Boyle R, and Tudor-Williams G
Subjects: medical education, pediatrics, self-confidence, medical students, Special aspects of education, LC8-6691, Medicine (General), R5-920
Abstract: Jhia Jiat Teh,1 Ka Yan Cheung,1 Yusuf Patrick,1 Mona Panahi,1 Robert Boyle,2 Gareth Tudor-Williams2 1Department of Medicine, Imperial College London, London, UK; 2Department of Pediatrics, Imperial College London, London, UKCorrespondence: Jhia Jiat TehSchool of Medicine, Imperial College London Exhibition Road, London SW7 2AZ, UKTel +44 74 2132 1772Email jhia.teh15@imperial.ac.ukBackground: Pediatrics is a specialty reserved until later stages of the medical curriculum, with many students receiving early exposure via volunteering opportunities. Self-perceived confidence across the pediatric curriculum is crucial, due to limited clinical exposure before qualification. We aimed to assess the impact of a 7-week pediatric placement on medical students’ self-perceived confidence and factors that influenced self-perceived confidence.Methods: We conducted a prospective pilot survey on three cohorts of fifth-year students undertaking pediatric placements in 2018. A two-part questionnaire was distributed before and after the placement, evaluating the level of self-confidence in clinical skills using a 10-point scale.Results: Of 103 students, 62 (60%) students completed both questionnaires. Of these, 34 (55%) students reported previous professional experiences with children. There was a significant increase in self-reported confidence scores across ten questions before (mean 5.4 [IQR 4.1– 6.1]) and after the placement (7.6 [6.6– 8.5], p< 0.0001). Subgroup analyses between students with prior professional experience with children and those without revealed a significant difference in preplacement confidence in four pediatric practices: verbal communication, physical engagement, asking sensitive or probing questions, and explaining medical management (p< 0.05). There was no significant difference in postplacement confidence between these two groups.Conclusion: Medical students with prior professional experience with children reported higher self-confidence in interacting with pediatric patients prior to placement. However, a large and consistent increase in confidence across the cohort was such that there were no measurable differences at exit. This study supports the value of undergraduate pediatric training in promoting student self-confidence in managing pediatric clinical issues.Keywords: medical education, pediatrics, self-confidence, medical students
Published: 2020

65. COVID-19 reinforces the need to improve sepsis care resources in Africa

Author: Nsutebu, E., Rylance, J., Appiah, J. A., Grobusch, M. P., Williams, G., Kissoon, N., Elfatih, M., Kabara, H. S., Osman, K. M., Reinhart, K., Mer, M., and Jacob, S.
Published: 2021
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66. On the Complementary Information Provided by Satellite Images, Lagrangian Drifters, and a Regional Numerical Model: a Case Study in the San Matias Gulf, Argentina

Author: Saraceno, M., Tonini, M. H., Williams, G. N., Aubone, N., Olascoaga, M. J., Beron-Vera, F. J., Gonzalez, R., Soria, M., Saad, J. F., and Svendsen, G.
Published: 2020
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67. Impact of Early Initiation of Eslicarbazepine Acetate on Economic Outcomes Among Patients with Focal Seizure: Results from Retrospective Database Analyses

Author: Mehta, Darshan, Davis, Matthew, Epstein, Andrew J., Wensel, Brian, Grinnell, Todd, and Williams, G. Rhys
Published: 2020
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68. Effects of dietary supplementation with vitamin E, selenium yeast or both on egg incubation response, embryonic development, keet quality, and posthatch growth of helmeted guinea fowl breeders

Author: Oso, A. O., Lala, O. A., Oke, E. O., Williams, G. A., Taiwo, A. G., and Ogunsola, Z. O.
Published: 2020
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69. The association of body composition parameters and adverse events in women receiving chemotherapy for early breast cancer

Author: Aleixo, G. F. P., Shachar, S. S., Deal, A. M., Nyrop, K. A., Muss, H. B., Chen, Y. T., Yu, H., and Williams, G. R.
Published: 2020
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70. Possible control of acute outbreaks of a marine fungal pathogen by nominally herbivorous tropical reef fish

Author: Neal, B. P., Honisch, B., Warrender, T., Williams, G. J., Work, T. M., and Price, N. N.
Published: 2020
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71. Association of body composition with function in women with early breast cancer

Author: Aleixo, G. F. P., Deal, A. M., Nyrop, K. A., Muss, H. B., Damone, E. M., Williams, G. R., Yu, H., and Shachar, S. S.
Published: 2020
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72. Direct Processing of Structural Thermoplastic Composites Using Rapid Isothermal Stamp Forming

Author: Reynolds, N., Awang-Ngah, S., Williams, G., and Hughes, D. J.
Published: 2020
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73. Possible very high transition temperatures in the infinite-layer ACuO$ _{2} $ cuprate superconductor for A={Mg, Ca, Sr, Ba}: A DFT study

Author: Mallett, B. P. P., Gaston, N., Storey, J. G., Williams, G. V. M., Kaiser, A. B., and Tallon, J. L.
Subjects: Condensed Matter - Superconductivity
Abstract: We show from a bond valence sum correlation that very high superconducting $ T_{c} $ values should be found in optimally hole-doped infinite-layer ACuO$ _{2} $ cuprates - up to 160~K for A = Ba. The projected increase in $ T_{c} $ across the series arises from "internal pressure" effects as A runs from Mg to Ba. We then use density functional theory to investigate these pressure effects on the band structure in an attempt to understand this progressive increase in $ T_{c} $. Where these materials have been synthesised we find good agreement between our calculated structural parameters and the experimental ones. We find that internal pressure associated with increasing ion size does indeed enhance the superconducting energy gap, as observed, via modifications to the electronic dispersion. Furthermore, in our calculations, pressure alters the dispersion independently of how it is applied (internal or external) so that the superconducting energy gap correlates with the unit-cell volume and a Fermi-surface shape-parameter describing ratio of next-nearest-neighbor to nearest-neighbor hopping integrals. We infer an energy scale for the pairing interaction of the order of 1~eV, well above the magnetic energy scale.
Published: 2013

74. Large low-temperature magnetoresistance in SrFe2As2 single crystals

Author: Chong, S. V., Williams, G. V. M., Kennedy, J., Fang, F., Tallon, J. L., and Kadowaki, K.
Subjects: Condensed Matter - Superconductivity
Abstract: We present the first report on a large low-temperature magnetoresistance (MR) of more than 1600% in a SrFe2As2 single crystal and 1300% in a low-energy Ca ion-implanted SrFe2As2 single crystal that occurs before the emergence of crystallographic strain-induced bulk superconductivity arising from a sample aging effect. In accordance to band structure calculations from literature, which consitently show more than 2 bands are involved in the transport, we have modeled this large MR at high fields using a 3-carrier scenario rather than solely on quantum linear MR model generally used to explain the MR in iron-pnictides. At and below 20 K the large MR may be due to 3-carrier transport in an inhomogeneous state where there are superconducting and metallic regions., Comment: 6 pages, 4 figures
Published: 2013
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75. GRB 091024A and the nature of ultra-long gamma-ray bursts

Author: Virgili, F. J., Mundell, C. G., Pal'shin, V., Guidorzi, C., Margutti, R., Melandri, A., Harrison, R., Kobayashi, S., Chornock, R., Henden, A., Updike, A. C., Cenko, S. B., Tanvir, N. R., Steele, I. A., Cucchiara, A., Gomboc, A., Levan, A., Cano, Z., Mottram, C. J., Clay, N. R., Bersier, D., Kopac, D., Japelj, J., Filippenko, A. V., Li, W., Svinkin, D., Golenetskii, S., Hartmann, D. H., Milne, P. A., Williams, G., O'Brien, P. T., Fox, D. B., and Berger, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a broadband study of gamma-ray burst (GRB) 091024A within the context of other ultra-long-duration GRBs. An unusually long burst detected by Konus-Wind, Swift, and Fermi, GRB 091024A has prompt emission episodes covering ~1300 s, accompanied by bright and highly structured optical emission captured by various rapid-response facilities, including the 2-m autonomous robotic Faulkes North and Liverpool Telescopes, KAIT, S-LOTIS, and SRO. We also observed the burst with 8- and 10-m class telescopes and determine the redshift to be z = 1.0924 \pm 0.0004. We find no correlation between the optical and gamma-ray peaks and interpret the optical light curve as being of external origin, caused by the reverse and forward shock of a highly magnetized jet (R_B ~ 100-200). Low-level emission is detected throughout the near-background quiescent period between the first two emission episodes of the Konus-Wind data, suggesting continued central-engine activity; we discuss the implications of this ongoing emission and its impact on the afterglow evolution and predictions. We summarize the varied sample of historical GRBs with exceptionally long durations in gamma-rays (>~ 1000 s) and discuss the likelihood of these events being from a separate population; we suggest ultra-long GRBs represent the tail of the duration distribution of the long GRB population., Comment: Updated abstract, acknowledgements. Accepted for publication in ApJ; 21 pages, 10 figures, 6 tables
Published: 2013
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76. DarkLight: A Search for Dark Forces at the Jefferson Laboratory Free-Electron Laser Facility

Author: Balewski, J., Bernauer, J., Bertozzi, W., Bessuille, J., Buck, B., Cowan, R., Dow, K., Epstein, C., Fisher, P., Gilad, S., Ihloff, E., Kahn, Y., Kelleher, A., Kelsey, J., Milner, R., Moran, C., Ou, L., Russell, R., Schmookler, B., Thaler, J., Tschalär, C., Vidal, C., Winnebeck, A., Benson, S., Gould, C., Biallas, G., Boyce, J. R., Coleman, J., Douglas, D., Ent, R., Evtushenko, P., Fenker, H. C., Gubeli, J., Hannon, F., Huang, J., Jordan, K., Legg, R., Marchlik, M., Moore, W., Neil, G., Shinn, M., Tennant, C., Walker, R., Williams, G., Zhang, S., Freytsis, M., Fiorito, R., O'Shea, P., Alarcon, R., Dipert, R., Ovanesyan, G., Gunter, T., Kalantarians, N., Kohl, M., Albayrak, I., Carmignotto, M., Horn, T., Gunarathne, D. S., Martoff, C. J., Olvitt, D. L., Surrow, B., Lia, X., Beck, R., Schmitz, R., Walther, D., Brinkmann, K., and Zaunig, H.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: We give a short overview of the DarkLight detector concept which is designed to search for a heavy photon A' with a mass in the range 10 MeV/c^2 < m(A') < 90 MeV/c^2 and which decays to lepton pairs. We describe the intended operating environment, the Jefferson Laboratory free electon laser, and a way to extend DarkLight's reach using A' --> invisible decays., Comment: 8 pages, 4 figures, contributed to the Community Summer Study 2013 "Snowmass on the Mississippi" in the New, Light, Weakly Coupled Particles (NLWCP) subgroup of the Intensity Frontier
Published: 2013

77. Transmission of High-Power Electron Beams Through Small Apertures

Author: Tschalaer, C., Alarcon, R., Balascuta, S., Benson, S. V., Bertozzi, W., Boyce, J. R., Cowan, R., Douglas, D., Evtushenko, P., Fisher, P., Ihloff, E., Kalantarians, N., Kelleher, A., Legg, R., Milner, R. G., Neil, G. R., Ou, L., Schmookler, B., Tennant, C., Williams, G. P., and Zhang, S.
Subjects: Physics - Accelerator Physics
Abstract: Tests were performed to pass a 100 MeV, 430 kWatt c.w. electron beam from the energy-recovery linac at the Jefferson Laboratory's FEL facility through a set of small apertures in a 127 mm long aluminum block. Beam transmission losses of 3 p.p.m. through a 2 mm diameter aperture were maintained during a 7 hour continuous run., Comment: arXiv admin note: text overlap with arXiv:1305.0199
Published: 2013
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78. Measured Radiation and Background Levels During Transmission of Megawatt Electron Beams Through Millimeter Apertures

Author: Alarcon, R., Balascuta, S., Benson, S. V., Bertozzi, W., Boyce, J. R., Cowan, R., Douglas, D., Evtushenko, P., Fisher, P., Ihloff, E., Kalantarians, N., Kelleher, A., Kossler, W. J., Legg, R., Long, E., Milner, R. G., Neil, G. R., Ou, L., Schmookler, B., Tennant, C., Tschalaer, C., Williams, G. P., and Zhang, S.
Subjects: Physics - Accelerator Physics
Abstract: We report measurements of photon and neutron radiation levels observed while transmitting a 0.43 MW electron beam through millimeter-sized apertures and during beam-off, but accelerating gradient RF-on, operation. These measurements were conducted at the Free-Electron Laser (FEL) facility of the Jefferson National Accelerator Laboratory (JLab) using a 100 MeV electron beam from an energy-recovery linear accelerator. The beam was directed successively through 6 mm, 4 mm, and 2 mm diameter apertures of length 127 mm in aluminum at a maximum current of 4.3 mA (430 kW beam power). This study was conducted to characterize radiation levels for experiments that need to operate in this environment, such as the proposed DarkLight Experiment. We find that sustained transmission of a 430 kW continuous-wave (CW) beam through a 2 mm aperture is feasible with manageable beam-related backgrounds. We also find that during beam-off, RF-on operation, multipactoring inside the niobium cavities of the accelerator cryomodules is the primary source of ambient radiation when the machine is tuned for 130 MeV operation., Comment: 9 pages, 11 figures, submitted to Nuclear Instruments and Methods in Physics Research Section A
Published: 2013
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79. Electron pockets and pseudogap asymmetry observed in the thermopower of underdoped cuprates

Author: Storey, J. G., Tallon, J. L., and Williams, G. V. M.
Subjects: Condensed Matter - Superconductivity
Abstract: We calculate the diffusion thermoelectric power of high-Tc cuprates using the resonating-valence-bond spin-liquid model developed by Yang, Rice and Zhang (YRZ). In this model, reconstruction of the energy-momentum dispersion results in a pseudogap in the density of states that is heavily asymmetric about the Fermi level. The subsequent asymmetry in the spectral conductivity is found to account for the large magnitude and temperature dependence of the thermopower observed in underdoped cuprates. In addition we find evidence in experimental data for electron pockets in the Fermi surface, arising from a YRZ-like reconstruction, near the onset of the pseudogap in the slightly overdoped regime., Comment: 6 pages, 7 figures, accepted for publication in EPL
Published: 2013
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80. Transmission of Megawatt Relativistic Electron Beams Through Millimeter Apertures

Author: Alarcon, R., Balascuta, S., Benson, S. V., Bertozzi, W., Boyce, J. R., Cowan, R., Douglas, D., Evtushenko, P., Fisher, P., Ihloff, E., Kalantarians, N., Kelleher, A., Legg, R., Milner, R. G., Neil, G. R., Ou, L., Schmookler, B., Tennant, C., Tschalaer, C., Williams, G. P., and Zhang, S.
Subjects: Physics - Accelerator Physics, High Energy Physics - Experiment, Nuclear Experiment
Abstract: High power, relativistic electron beams from energy recovery linacs have great potential to realize new experimental paradigms for pioneering innovation in fundamental and applied research. A major design consideration for this new generation of experimental capabilities is the understanding of the halo associated with these bright, intense beams. In this Letter, we report on measurements performed using the 100 MeV, 430 kWatt CW electron beam from the energy recovery linac at the Jefferson Laboratory's Free Electron Laser facility as it traversed a set of small apertures in a 127 mm long aluminum block. Thermal measurements of the block together with neutron measurements near the beam-target interaction point yielded a consistent understanding of the beam losses. These were determined to be 3 ppm through a 2 mm diameter aperture and were maintained during a 7 hour continuous run., Comment: 10 pages, 5 figures
Published: 2013
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81. Microcoulomb (0.7 ± 0.40.2 μC) laser plasma accelerator on OMEGA EP

Author: Shaw, J. L., Romo-Gonzalez, M. A., Lemos, N., King, P. M., Bruhaug, G., Miller, K. G., Dorrer, C., Kruschwitz, B., Waxer, L., Williams, G. J., Ambat, M. V., McKie, M. M., Sinclair, M. D., Mori, W. B., Joshi, C., Chen, Hui, Palastro, J. P., Albert, F., and Froula, D. H.
Published: 2021
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82. Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126

Author: Henze, M., Pietsch, W., Haberl, F., Della Valle, M., Riffeser, A., Sala, G., Hatzidimitriou, D., Hofmann, F., Hartmann, D. H., Koppenhoefer, J., Seitz, S., Williams, G. G., Hornoch, K., Itagaki, K., Kabashima, F., Nishiyama, K., Xing, G., Lee, C. H., Magnier, E., and Chambers, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: [Abridged] Classical novae (CNe) represent the main class of supersoft X-ray sources (SSSs) in the central region of our neighbouring galaxy M 31. Only three confirmed novae and three SSSs have been discovered in globular clusters (GCs) of any galaxy so far, of which one nova and two SSSs (including the nova) were found in M 31 GCs. To study the SSS state of CNe we carried out a high-cadence X-ray monitoring of the M 31 central area with XMM-Newton and Chandra. We analysed X-ray and optical data of a new transient X-ray source in the M 31 GC Bol 126, discovered serendipitously in Swift observations. Our optical data set was based on regular M 31 monitoring programmes from five different small telescopes. Additionally, we made use of Pan-STARRS 1 data obtained during the PAndromeda survey. Our observations reveal that the X-ray source in Bol 126 is the third SSS in an M 31 GC and can be confirmed as the second CN in the M 31 GC system. This nova is named M31N 2010-10f. Its properties in the X-ray and optical regimes agree with a massive white dwarf (M_WD >~ 1.3 M_sun) in the binary system. Incorporating the data on previously found (suspected) novae in M 31 GCs we used our high-cadence X-ray monitoring observations to estimate a tentative nova rate in the M 31 GC system of 0.05 /yr/GC. An optical estimate, based on the recent 10.5-year WeCAPP survey, gives a lower nova rate, which is compatible with the X-ray rate on the 95% confidence level. There is growing evidence that the nova rate in GCs is higher than expected from primordial binary formation and under conditions as in the field. Dynamical binary formation and/or additional accretion from the intracluster medium are possible scenarios for an increased nova rate, but observational confirmation for this enhancement has been absent, so far. Regular X-ray monitoring observations of M 31 provide a promising strategy to find these novae., Comment: 14 pages, 6 figures, 3 tables; accepted by Astronomy and Astrophysics
Published: 2012
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83. Dielectric versus magnetic pairing mechanisms in high-temperature cuprate superconductors investigated using Raman scattering

Author: Mallett, B. P. P., Wolf, T., Gilioli, E., Licci, F., Williams, G. V. M., Kaiser, A. B., Suresh, N., Ashcroft, N. W., and Tallon, J. L.
Subjects: Condensed Matter - Superconductivity
Abstract: We suggest, and demonstrate, a systematic approach to the study of cuprate superconductors, namely, progressive change of ion size in order to systematically alter the interaction strength and other key parameters. R(Ba,Sr)$_2$Cu$_3$O$_y$ (R={La, ... Lu,Y}) is such a system where potentially obscuring structural changes are minimal. We thereby systematically alter both dielectric and magnetic properties. Dielectric fluctuation is characterized by ionic polarizability while magnetic fluctuation is characterized by exchange interactions measurable by Raman scattering. The range of transition temperatures is 70 to 107 K and we find that these correlate only with the dielectric properties, a behavior which persists with external pressure. The ultimate significance may remain to be proven but it highlights the role of dielectric screening in the cuprates and adds support to a previously proposed novel pairing mechanism involving exchange of quantized waves of electronic polarization., Comment: Manuscript: 5 pages, 4 figures. Supplemental material included (9 pages, 5 figures)
Published: 2012
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84. Tc is insensitive to magnetic interactions in high-Tc superconductors

Author: Mallett, B., Williams, G. V. M., Kaiser, A. B., Gilioli, E., Licci, F., Wolf, T., and Tallon, J. L.
Subjects: Condensed Matter - Superconductivity
Abstract: A quarter of a century after their discovery the mechanism that pairs carriers in the cuprate high-Tc superconductors (HTS) still remains uncertain. Despite this the general consensus is that it is probably magnetic in origin [1] so that the energy scale for the pairing boson is governed by J, the antiferromagnetic exchange interaction. Recent studies using resonant inelastic X-ray scattering strongly support these ideas [2]. Here as a further test we vary J (as measured by two-magnon Raman scattering) by more than 60% by changing ion sizes in the model HTS system LnA2Cu3O7-{\delta} where A=(Ba,Sr) and Ln=(La, Nd, Sm, Eu, Gd, Dy, Yb, Lu). Such changes are often referred to as "internal" pressure. Surprisingly, we find Tcmax anticorrelates with J where internal pressure is the implicit variable. This is the opposite to the effect of external pressure and suggests that J is not the dominant energy scale governing Tcmax., Comment: 8 pages, 3 figures
Published: 2012

85. Multi-epoch Spectropolarimetry of SN 2011fe

Author: Smith, Paul S., Williams, G. Grant, Smith, Nathan, Milne, Peter A., Jannuzi, Buell T., and Green, E. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We present multiple spectropolarimetric observations of the nearby Type Ia supernova SN 2011fe in M101, obtained before, during, and after the time of maximum apparent visual brightness. SN 2011fe exhibits time-dependent polarization in both the continuum and strong absorption lines. At all epochs, red wavelengths exhibit a degree of continuum polarizaiton of 0.2-0.4 per cent, likely indicative of persistent asymmetry in the electron-scattering photosphere. However, the degree of polarization across the Si II 6355 absorption line varies dramatically from epoch to epoch. Before maximum, Si II 6355 shows enhanced polarization at the same position angle (PA) as the polarized continuum. During two epochs near maximum, however, Si II 6355 absorption has a lower degree of polarization, with a PA that is 90deg from the continuum. After maximum, the absorption feature has the same degree of polarization and PA as the adjacent continuum. Another absorption feature in the blue (either Si II 5051 or a blend with Fe II lines) shows qualitatively similar changes, although the changes are shifted in time to an earlier epoch. This behavior is similar to that seen in broad absorption-line quasars, where the polarization in absorption features has been interpreted as the line absorbing some of the unpolarized continuum flux. This behavior, along with the 90deg shifts of the polarization PA with time, imply a time-dependent large-scale asymmetry in the explosion., Comment: 5 pages, 3 color figures, submitted to ApJ Letters
Published: 2011

86. Coherence Properties of Individual Femtosecond Pulses of an X-ray Free-Electron Laser

Author: Vartanyants, I. A., Singer, A., Mancuso, A. P., Yefanov, O., Sakdinawat, A., Liu, Y., Bang, E., Williams, G. J., Cadenazzi, G., Abbey, B., Sinn, H., Attwood, D., Nugent, K. A., Weckert, E., Wang, T., Zhu, D., Wu, B., Graves, C., Scherz, A., Turner, J. J., Schlotter, W. F., Messerschmidt, M., Luning, J., Acremann, Y., Heimann, P., Mancini, D. C., Joshi, V., Krzywinski, J., Soufli, R., Fernandez-Perea, M., Hau-Riege, S., Peele, A. G., Feng, Y., Krupin, O., Moeller, S., and Wurth, W.
Subjects: Physics - Optics
Abstract: Measurements of the spatial and temporal coherence of single, femtosecond x-ray pulses generated by the first hard x-ray free-electron laser (FEL), the Linac Coherent Light Source (LCLS), are presented. Single shot measurements were performed at 780 eV x-ray photon energy using apertures containing double pinholes in "diffract and destroy" mode. We determined a coherence length of 17 micrometers in the vertical direction, which is approximately the size of the focused LCLS beam in the same direction. The analysis of the diffraction patterns produced by the pinholes with the largest separation yields an estimate of the temporal coherence time of 0.6 fs. We find that the total degree of transverse coherence is 56% and that the x-ray pulses are adequately described by two transverse coherent modes in each direction. This leads us to the conclusion that 78% of the total power is contained in the dominant mode., Comment: 6 pages, 4 figures
Published: 2011
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87. Monster in the Dark: The Ultraluminous GRB 080607 and its Dusty Environment

Author: Perley, Daniel A., Morgan, A. N., Updike, A., Yuan, F., Akerlof, C. W., Miller, A. A., Bloom, J. S., Cenko, S. B., Li, W., Filippenko, A. V., Prochaska, J. X., Kann, D. A., Butler, N. R., Christian, P., Hartmann, D. H., Milne, P., Rykoff, E. S., Rujopakarn, W., Wheeler, J. C., and Williams, G. G.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present early-time optical through infrared photometry of the bright gamma-ray burst GRB 080607, starting only 6 s following the initial trigger in the rest frame. Complemented by our previously published spectroscopy, this high-quality photometric dataset allows us to solve for the extinction properties of the redshift 3.036 sightline, giving perhaps the most detailed information on the ultraviolet continuum absorption properties of any sightline outside our Local Group to date. The extinction properties are not adequately modeled by any ordinary extinction template (including the average Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud curves), partially because the 2175-Angstrom feature (while present) is weaker by about a factor of two than when seen under similar circumstances locally. However, the spectral energy distribution is exquisitely fitted by the more general Fitzpatrick & Massa (1990) parameterization of Local-Group extinction, putting it in the same family as some peculiar Milky Way extinction curves. After correcting for this (considerable, A_V = 3.3 +/- 0.4 mag) extinction, GRB 080607 is revealed to have been among the most optically luminous events ever observed, comparable to the naked-eye burst GRB 080319B. Its early peak time (t_rest < 6 s) indicates a high initial Lorentz factor (Gamma > 600), while the extreme luminosity may be explained in part by a large circumburst density. Only because of its early high luminosity could the afterglow of GRB 080607 be studied in such detail in spite of the large attenuation and great distance, making this burst an excellent prototype for the understanding of other highly obscured extragalactic objects, and of the class of "dark" GRBs in particular., Comment: Submitted to AJ. 15 pages, 6 tables, 9 figures
Published: 2010
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88. Studying the Underlying Event in Drell-Yan and High Transverse Momentum Jet Production at the Tevatron

Author: The CDF Collaboration, Aaltonen, T., Adelman, J., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Attal, A., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauer, G., Beauchemin, P. -H., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Berge, D., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Blair, R. E., Blocker, C., Blumenfeld, B., Bocci, A., Bodek, A., Boisvert, V., Bortoletto, D., Boudreau, J., Boveia, A., Brau, B., Bridgeman, A., Brigliadori, L., Bromberg, C., Brubaker, E., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Byrum, K. L., Cabrera, S., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Canepa, A., Carls, B., Carlsmith, D., Carosi, R., Carrillon, S., Carron, S., Casal, B., Casarsa, M., Castrocc, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chang, S. H., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chungo, K., Chung, W. H., Chung, Y. S., Chwalek, T., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clark, D., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Cully, J. C., Dagenhart, D., Datta, M., Davies, T., de Barbaro, P., De Cecco, S., Deisher, A., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., d'Errico, M., Di Canto, A., di Giovanni, G. P., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, T., Dube, S., Ebina, K., Elagin, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Fedorko, W. T., Feild, R. G., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagans, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Furic, I., Gallinaro, M., Galyardt, J., Garberson, F., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerdes, D., Gessler, A., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Gimmell, J. L., Ginsburg, C. M., Giokaris, N., Giordani, M., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., González, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Gresele, A., Grinstein, S., Grosso-Pilcher, C., Group, R. C., Grundler, U., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Han, B. -Y., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hartz, M., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Heuser, J., Hewamanage, S., Hickman, M., Hidas, D., Hill, C. S., Hirschbuehl, D., Hocker, A., Hou, S., Houlden, M., Hsu, S. -C., Hughes, R. E., Hurwitz, M., Husemann, U., Hussein, M., Huston, J., Incandela, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Jung, J. E., Junk, T. R., Kamon, T., Kar, D., Karchin, P. E., Kato, Y., Kephart, R., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirsch, L., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Korytov, A., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kulkarni, N. P., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., Lazzizzera, I., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leone, S., Lewis, J. D., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, T., Lockyer, N. S., Loginov, A., Lovas, L., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., MacQueen, D., Madrak, R., Maeshima, K., Makhoul, K., Maksimovic, P., Malde, S., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Marino, C. P., Martin, A., Martink, V., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mathis, M., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Miladinovic, N., Miller, R., Mills, C., Milnik, M., Mitra, A., Mitselmakher, G., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mulmenstadt, J., Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakamura, K., Nakano, Napier, A., Nett, J., Neu, C., Neubauer, M. S., Neubauer, S., Nielseng, J., Nodulman, L., Norman, M., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Osterberg, K., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Papaikonomou, A., Paramanov, A. A., Parks, B., Pashapour, S., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Peiffer, T., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pinera, L., Pitts, K., Plager, C., Pondrom, L., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rademacker, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Redondo, I., Renton, P., Renz, M., Rescigno, M., Richter, S., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rossin, R., Roy, P., Ruiz, A., Russ, J., Rusu, V., Rutherford, B., Saarikko, H., Safonov, A., Sakumoto, W. K., Santi, L., Sartori, L., Sato, K., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. A., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sexton-Kennedy, L., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shon, Y., Shreyber, I., Simonenko, A., Sinervo, P., Sisakyan, A., Slaughter, A. J., Slaunwhite, J., Sliwa, K., Smith, J. R., Snider, F. D., Snihur, R., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Suh, J. S., Sukhanov, A., Suslov, I., Taffard, A., Takashima, R., Takeuchi, Y., Tanaka, R., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Tipton, P., Ttito-Guzmán, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Tourneur, S., Trovato, M., Tsai, S. -Y., Tu, Y., Turiniff, N., Ukegawa, F., Uozumi, S., van Remortel, N., Varganov, A., Vataga, E., Vázquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vogel, M., Volobouev, I., Volpi, G., Wagner, P., Wagner, R. G., Wagner, R. L., Wagner, W., Wagner-Kuhr, J., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Weinelt, J., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Williams, G., Williams, H. H., Wilson, M. G., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, C., Wolfe, H., Wright, T., Wu, X., Würthwein, F., Yagil, A., Yamamoto, K., Yamaoka, J., Yang, U. K., Yang, Y. C., Yao, W. M., Yeh, G. P., Yio, K., Yoh, J., Yorita, K., Yoshidal, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., Zhang, X., Zheng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: We study the underlying event in proton-antiproton collisions by examining the behavior of charged particles (transverse momentum pT > 0.5 GeV/c, pseudorapidity |\eta| < 1) produced in association with large transverse momentum jets (~2.2 fb-1) or with Drell-Yan lepton-pairs (~2.7 fb-1) in the Z-boson mass region (70 < M(pair) < 110 GeV/c2) as measured by CDF at 1.96 TeV center-of-mass energy. We use the direction of the lepton-pair (in Drell-Yan production) or the leading jet (in high-pT jet production) in each event to define three regions of \eta-\phi space; toward, away, and transverse, where \phi is the azimuthal scattering angle. For Drell-Yan production (excluding the leptons) both the toward and transverse regions are very sensitive to the underlying event. In high-pT jet production the transverse region is very sensitive to the underlying event and is separated into a MAX and MIN transverse region, which helps separate the hard component (initial and final-state radiation) from the beam-beam remnant and multiple parton interaction components of the scattering. The data are corrected to the particle level to remove detector effects and are then compared with several QCD Monte-Carlo models. The goal of this analysis is to provide data that can be used to test and improve the QCD Monte-Carlo models of the underlying event that are used to simulate hadron-hadron collisions., Comment: Submitted to Phys.Rev.D
Published: 2010
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89. Evidence for Supernova-Synthesised Dust from the Rising Afterglow of GRB 071025 at z~5

Author: Perley, Daniel A., Bloom, J. S., Klein, C. R., Covino, S., Minezaki, T., Wozniak, P., Vestrand, W. T., Williams, G. G., Milne, P., Butler, N. R., Updike, A. C., Krühler, T., Afonso, P., Antonelli, A., Cowie, L., Ferrero, P., Greiner, J., Hartmann, D. H., Kakazu, Y., Yoldas, A. Küpcü, Morgan, A. N., Price, P. A., Prochaska, J. X., and Yoshii, Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present observations and analysis of the broadband afterglow of Swift GRB 071025. Using optical and infrared (RIYJHK) photometry, we derive a photometric redshift of 4.4 < z < 5.2; at this redshift our simultaneous multicolour observations begin at ~30 s after the GRB trigger in the host frame and during the initial rising phase of the afterglow. We associate the light curve peak at 580 s in the observer frame with the formation of the forward shock, giving an estimate of the initial Lorentz factor Gamma_0 ~ 200. The red spectral energy distribution (even in regions not affected by the Lyman-alpha break) provides secure evidence of a large dust column. However, the inferred extinction curve shows a prominent flat component between 2000-3000 Angstroms in the rest-frame, inconsistent with any locally observed template but well-fit by models of dust formed by supernovae. Time-dependent fits to the extinction profile reveal no evidence of dust destruction and limit the decrease in the extinction column to Delta A_3000 < 0.54 mag after t = 50 s in the rest frame. Our observations provide evidence of a transition in dust properties at z~5, in agreement with studies of high-z quasars, and suggest that SN-formed dust continues to dominate the opacity of typical galaxies at this redshift., Comment: Resubmitted to MNRAS following referee report. Contains additional figure and some extra analysis/discussion
Published: 2009
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90. Synchronous Optical and Radio Polarization Variability in the Blazar OJ287

Author: D'Arcangelo, F. D., Marscher, A. P., Jorstad, S. G., Smith, P. S., Larionov, V. M., Hagen-Thorn, V. A., Williams, G. G., Gear, W. K., Clemens, D. P., Sarcia, D., Grabau, A., Tollestrup, E. V., Buie, M. W., Taylor, B., and Dunham, E.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We explore the variability and cross-frequency correlation of the flux density and polarization of the blazar OJ287, using imaging at 43 GHz with the Very Long Baseline Array, as well as optical and near-infrared polarimetry. The polarization and flux density in both the optical waveband and the 43 GHz compact core increased by a small amount in late 2005, and increased significantly along with the near-IR polarization and flux density over the course of 10 days in early 2006. Furthermore, the values of the electric vector position angle (EVPA) at the three wavebands are similar. At 43 GHz, the EVPA of the blazar core is perpendicular to the flow of the jet, while the EVPAs of emerging superluminal knots are aligned parallel to the jet axis. The core polarization is that expected if shear aligns the magnetic field at the boundary between flows of disparate velocities within the jet. Using variations in flux density, percentage polarization, and EVPA, we model the inner jet as a spine-sheath system. The model jet contains a turbulent spine of half-width 1.2 degrees and maximum Lorentz factor of 16.5, a turbulent sheath with Lorentz factor of 5, and a boundary region of sheared field between the spine and sheath. Transverse shocks propagating along the fast, turbulent spine can explain the superluminal knots. The observed flux density and polarization variations are then compatible with changes in the direction of the inner jet caused by a temporary change in the position of the core if the spine contains wiggles owing to an instability. In addition, we can explain a stable offset of optical and near-IR percentage polarization by a steepening of spectral index with frequency, as supported by the data., Comment: 34 pages, 12 figures; To be published in Astrophysical Journal, accepted 03/2009
Published: 2009
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91. Thermoelectric power of high-Tc superconductors calculated from the electronic structure

Author: Storey, J. G., Tallon, J. L., and Williams, G. V. M.
Subjects: Condensed Matter - Superconductivity
Abstract: We have calculated the thermopower of the Bi2Sr2CuO6 and Bi2Sr2CaCu2O8 superconductors using an ARPES-derived dispersion, with a model pseudogap, and a marginal-Fermi liquid scattering rate that has a minimum with respect to energy at the van Hove singularity (vHs). Good fits with data are achieved across the entire phase diagram, thus confirming the dispersions, the locations of the vHs and the dominance of the diffusion thermopower over the phonon drag contribution., Comment: 5 pages, 7 figures, submitted to Physical Review B as a Rapid Communication
Published: 2009

92. The very short supersoft X-ray state of the classical nova M31N 2007-11a

Author: Henze, M., Pietsch, W., Sala, G., Della Valle, M., Hernanz, M., Greiner, J., Burwitz, V., Freyberg, M. J., Haberl, F., Hartmann, D. H., Milne, P., and Williams, G. G.
Subjects: Astrophysics
Abstract: Short supersoft X-ray source (SSS) states (durations < 100 days) of classical novae (CNe) indicate massive white dwarfs that are candidate progenitors of supernovae type Ia. We carry out a dedicated optical and X-ray monitoring program of CNe in the bulge of M 31. We discovered M31N 2007-11a and determined its optical and X-ray light curve. We used the robotic Super-LOTIS telescope to obtain the optical data and XMM-Newton and Chandra observations to discover an X-ray counterpart to that nova. Nova M31N 2007-11a is a very fast CN, exhibiting a very short SSS state with an appearance time of 6-16 days after outburst and a turn-off time of 45-58 days after outburst. The optical and X-ray light curves of M31N 2007-11a suggest a binary containing a white dwarf with a mass greater than one solar mass., Comment: 4 pages, 2 figures, 2 tables, submitted to A&A Letters; v2: accepted version
Published: 2008
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93. The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Author: Henze, M., Pietsch, W., Haberl, F., Sala, G., Quimby, R., Hernanz, M., Della Valle, M., Milne, P., Williams, G. G., Burwitz, V., Greiner, J., Stiele, H., Hartmann, D. H., Kong, A. K. H., and Hornoch, K.
Subjects: Astrophysics
Abstract: Classical novae (CNe) have been found to represent the major class of supersoft X-ray sources (SSS) in our neighbour galaxy M 31. We determine properties and evolution of the two first SSSs ever discovered in the M 31 globular cluster (GC) system. We have used XMM-Newton, Chandra and Swift observations of the centre region of M 31 to discover both SSS and to determine their X-ray light curves and spectra. We performed detailed analysis of XMM-Newton EPIC PN spectra of the source in Bol 111 (SS1) using blackbody and NLTE white dwarf (WD) atmosphere models. For the SSS in Bol 194 (SS2) we used optical monitoring data to search for an optical counterpart. Both GC X-ray sources were classified as SSS. We identify SS1 with the CN M31N 2007-06b recently discovered in the M 31 GC Bol 111. For SS2 we did not find evidence for a recent nova outburst and can only provide useful constraints on the time of the outburst of a hypothetical nova. The only known CN in a M 31 GC can be identified with the first SSS found in a M31 GC. We discuss the impact of our observations on the nova rate for the M 31 GC system., Comment: 11 pages, 9 figures, 4 tables, submitted to A&A; v2: accepted version
Published: 2008
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94. Impact of serratus plane block on pain scores and incentive spirometry volumes after chest trauma

Author: Hernandez N, de Haan J, Clendeninn D, Meyer DE, Ghebremichael S, Artime C, Williams G, Eltzschig H, and Sen S
Subjects: Polytrauma, Rib fractures, pain management, regional anesthesia, Anesthesiology, RD78.3-87.3
Abstract: Nadia Hernandez,1 Johanna de Haan,1 Dallis Clendeninn,1 David E Meyer,2 Semhar Ghebremichael,1 Carlos Artime,1 George Williams,1 Holger Eltzschig,1 Sudipta Sen11Department of Anesthesiology, Houston’s McGovern Medical School, University of Texas Health Science Center, Houston, TX, 77030, USA; 2Department of Surgery, Houston’s McGovern Medical School, University of Texas Health Science Center, Houston, TX, 77030, USABackground: Adequate pain control is difficult to achieve in patients with multiple rib fractures (MRF). Serratus plane block (SPB) is a novel technique for alleviating rib fracture pain. Several published case reports support this hypothesis.Purpose: The purpose of this study was to evaluate the use of SPB in MRF at our level 1 trauma center.Methods: Our hospital’s Regional Anesthesia Registry was queried for all trauma patients with MRF who underwent SPB between August 2014 and January 2018. Data were compared in each patient as a matched pair for the time periods before and after undergoing SPB. Thirty-four patients with similar baseline characteristics were enrolled.Results: The median number of rib fractures was 7. Ordinal pain scores were found to be improved 4 hrs after SPB from median 7/10 to 3/10 (P
Published: 2019

95. From Shock Breakout to Peak and Beyond: Extensive Panchromatic Observations of the Type Ib Supernova 2008D associated with Swift X-ray Transient 080109

Author: Modjaz, Maryam, Li, W., Butler, N., Chornock, R., Perley, D., Blondin, S., Bloom, J. S., Filippenko, A. V., Kirshner, R. P., Kocevski, D., Poznanski, D., Hicken, M., Foley, R. J., Stringfellow, G. S., Berlind, P., Navascues, D. Barrado y, Blake, C. H., Bouy, H., Brown, W. R., Challis, P., Chen, H., de Vries, W. H., Dufour, P., Falco, E., Friedman, A., Ganeshalingam, M., Garnavich, P., Holden, B., Illingworth, G., Liebert, J., Marion, G. H., Lee, N., Olivier, S. S., Prochaska, J. X., Silverman, J. M., Smith, N., Starr, D., Steele, T. N., Stockton, A., Williams, G. G., and Wood-Vasey, W. M.
Subjects: Astrophysics
Abstract: We present extensive early photometric (ultraviolet through near-infrared) and spectroscopic (optical and near-infrared) data on supernova (SN) 2008D as well as X-ray data analysis on the associated Swift/X-ray transient (XRT) 080109. Our data span a time range of 5 hours before the detection of the X-ray transient to 150 days after its detection, and detailed analysis allowed us to derive constraints on the nature of the SN and its progenitor; throughout we draw comparisons with results presented in the literature and find several key aspects that differ. We show that the X-ray spectrum of XRT 080109 can be fit equally well by an absorbed power law or a superposition of about equal parts of both power law and blackbody. Our data first established that SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous He lines), and show that SN 2008D had a relatively long rise time of 18 days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for \Delta t~0.1- 4 day, most pronounced in the blue bands) followed by 56^Ni decay. We construct a reliable measurement of the bolometric output for this stripped-envelope SN, and, combined with estimates of E_K and M_ej from the literature, estimate the stellar radius R_star of its probable Wolf-Rayet progenitor. According to the model of Waxman et al. and of Chevalier & Fransson, we derive R_star^{W07}= 1.2+/-0.7 R_sun and R_star^{CF08}= 12+/-7 R_sun, respectively; the latter being more in line with typical WN stars. Spectra obtained at 3 and 4 months after maximum light show double-peaked oxygen lines that we associate with departures from spherical symmetry, as has been suggested for the inner ejecta of a number of SN Ib cores., Comment: Accepted to ApJ, v3 contains more data than v2 and more references, conclusions not significantly changed, 28 pages in emulateapj, 17 figures
Published: 2008
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96. The Rapidly Flaring Afterglow of the Very Bright and Energetic GRB 070125

Author: Updike, Adria C., Haislip, Joshua B., Nysewander, Melissa C., Fruchter, Andrew S., Kann, D. Alexander, Klose, Sylvio, Milne, Peter A., Williams, G. Grant, Zheng, Weikang, Hergenrother, Carl W., Prochaska, Jason X., Halpern, Jules P., Mirabal, Nestor, Thorstensen, John R., van der Horst, Alexander J., Starling, Rhaana L. C., Racusin, Judith L., Burrows, David N., Kuin, N. P. M., Roming, Peter W. A., Bellm, Eric, Hurley, Kevin, Li, Weidong, Filippenko, Alexei V., Blake, Cullen, Starr, Dan, Falco, Emilio E., Brown, Warren R., Dai, Xinyu, Deng, Jinsong, Xin, Liping, Qiu, Yulei, Wei, Jianyan, Urata, Yuji, Nanni, Domenico, Maiorano, Elisabetta, Palazzi, Eliana, Greco, Giuseppe, Bartolini, Corrado, Guarnieri, Adriano, Piccioni, Adalberto, Pizzichini, Graziella, Terra, Federica, Misra, Kuntal, Bhatt, B. C., Anupama, G. C., Fan, X., Jiang, L., Wijers, Ralph A. M. J., Reichart, Dan E., Eid, Hala A., Bryngelson, Ginger, Puls, Jason, Goldthwaite, R. C., and Hartmann, Dieter H.
Subjects: Astrophysics
Abstract: We report on multi-wavelength observations, ranging from the X-ray to radio wave bands, of the IPN-localized gamma-ray burst GRB 070125. Spectroscopic observations reveal the presence of absorption lines due to O I, Si II, and C IV, implying a likely redshift of z = 1.547. The well-sampled light curves, in particular from 0.5 to 4 days after the burst, suggest a jet break at 3.7 days, corresponding to a jet opening angle of ~7.0 degrees, and implying an intrinsic GRB energy in the 1 - 10,000 keV band of around E = (6.3 - 6.9)x 10^(51) erg (based on the fluences measured by the gamma-ray detectors of the IPN network). GRB 070125 is among the brightest afterglows observed to date. The spectral energy distribution implies a host extinction of Av < 0.9 mag. Two rebrightening episodes are observed, one with excellent time coverage, showing an increase in flux of 56% in ~8000 seconds. The evolution of the afterglow light curve is achromatic at all times. Late-time observations of the afterglow do not show evidence for emission from an underlying host galaxy or supernova. Any host galaxy would be subluminous, consistent with current GRB host-galaxy samples. Evidence for strong Mg II absorption features is not found, which is perhaps surprising in view of the relatively high redshift of this burst and the high likelihood for such features along GRB-selected lines of sight., Comment: 50 pages, 9 figures, 5 tables Accepted to the Astrophysical Journal
Published: 2008
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97. Near-Zero Moment Ferromagnetism in the Semiconductor SmN

Author: Meyer, C., Ruck, B. J., Zhong, J., Granville, S., Preston, A. R. H., Williams, G. V. M., and Trodahl, H. J.
Subjects: Condensed Matter - Strongly Correlated Electrons
Abstract: The magnetic behaviour of SmN has been investigated in stoichiometric polycrystalline films. All samples show ferromagnetic order with Curie temperature (T_c) of 27 +/- 3 K, evidenced by the occurrence of hysteresis below T_c. The ferromagnetic state is characterised by a very small moment and a large coercive field, exceeding even the maximum applied field of 6 T below about 15 K. The residual magnetisation at 2 K, measured after cooling in the maximum field, is 0.035 mu_B per Sm. Such a remarkably small moment results from a near cancellation of the spin and orbital contributions for Sm3+ in SmN. Coupling to an applied field is therefore weak, explaining the huge coercive field . The susceptibility in the paramagnetic phase shows temperature-independent Van Vleck and Curie-Weiss contributions. The Van Vleck contribution is in quantitative agreement with the field-induced admixture of the J=7/2 excited state and the 5/2 ground state. The Curie-Weiss contribution returns a Curie temperature that agrees with the onset of ferromagnetic hysteresis, and a conventional paramagnetic moment with an effective moment of 0.4 mu_B per Sm ion, in agreement with expectations for the crystal-field modified effective moment on the Sm3+ ions., Comment: 5 pages, 3 figures
Published: 2008
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98. The pseudogap ground state in high temperature superconductors

Author: Storey, J. G., Tallon, J. L., and Williams, G. V. M.
Subjects: Condensed Matter - Superconductivity
Abstract: By re-examining recently-published data from angle-resolved photoemission spectroscopy we demonstrate that, in the superconducting region of the phase diagram, the pseudogap ground state is an arc metal. This scenario is consistent with results from Raman spectroscopy, specific heat and NMR. In addition, we propose an explanation for the "Fermi pockets" inferred from quantum oscillations in terms of a pseudogapped bilayer Fermi surface., Comment: 4 pages, 3 figures, added discussion of NMR and optical conductivity data, submitted to Physical Review B as a rapid communication
Published: 2008
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99. The Robotic Super-LOTIS Telescope: Results & Future Plans

Author: Williams, G. G., Milne, P. A., Park, H. S., Barthelmy, S. D., Hartmann, D. H., Updike, A., and Hurley, K.
Subjects: Astrophysics
Abstract: We provide an overview of the robotic Super-LOTIS (Livermore Optical Transient Imaging System) telescope and present results from gamma-ray burst (GRB) afterglow observations using Super-LOTIS and other Steward Observatory telescopes. The 0.6-m Super-LOTIS telescope is a fully robotic system dedicated to the measurement of prompt and early time optical emission from GRBs. The system began routine operations from its Steward Observatory site atop Kitt Peak in April 2000 and currently operates every clear night. The telescope is instrumented with an optical CCD camera and a four position filter wheel. It is capable of observing Swift Burst Alert Telescope (BAT) error boxes as early or earlier than the Swift UV/Optical Telescope (UVOT). Super-LOTIS complements the UVOT observations by providing early R- and I-band imaging. We also use the suite of Steward Observatory telescopes including the 1.6-m Kuiper, the 2.3-m Bok, the 6.5-m MMT, and the 8.4-m Large Binocular Telescope to perform follow-up optical and near infrared observations of GRB afterglows. These follow-up observations have traditionally required human intervention but we are currently working to automate the 1.6-m Kuiper telescope to minimize its response time., Comment: 4 pages, submitted to the proceedings of Gamma Ray Bursts 2007, Santa Fe, New Mexico, November 5-9 2007
Published: 2008
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100. Pressure dependence of the oxygen isotope effect in YBa$_2$Cu$_4$O$_8$

Author: Suresh, N., Storey, J. G., Williams, G. V. M., and Tallon, J. L.
Subjects: Condensed Matter - Superconductivity
Abstract: We have carried out measurements of the pressure dependence to 1.2 GPa of the oxygen isotope effect on $T_c$ in the high-$T_c$ superconductor YBa$_2$Cu$_4$O$_8$ using a clamp cell in a SQUID magnetometer. This compound lies close to, but just above, the 1/8$^{th}$ doping point where in La$_{2-x}$Sr$_x$CuO$_4$ marked anomalies in isotope effects occur. Both isotopes show the same very large pressure dependence of $T_c$ with the result that the isotope exponent remains low ($\sim$0.08) but increases slightly with increasing pressure. This is discussed in terms of stripe suppression, a competing pseudogap and the effect of superconducting fluctuations., Comment: 4 pages, 1 figures, submitted to Phys. Rev. B
Published: 2007
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