383 research outputs found
UA94/5/1 Beta Omega Chi Dance Card
No full textBeta Omega Chi dance program and card for the spring formal belonging to George Wells. Includes program, menu, list of members and officers, Beta Omega Chi song lyrics and dance card
Chi Omega Sorority Chapter Facility Exterior
No full textFront facing image of Chi Omega (Chi O). Located at 1145 N. Mountain. Chi Omega, originally founded at the University of Arkansas in 1895, founded at the University of Arizona in 1922 as the Zeta Beta Chapter. The building remains on 1145 N. Mountain, now as a University building a part of the College of Law. Chi Omega relocated to 1420 E. 1st St
Cross section measurements of e(+) e(-) -> omega chi(c0) from root s=4.178 to 4.278 GeV
No full textKolcu, Onur Buğra (Arel Author)The cross section of the process e(+)e(-) -> omega chi(C0) is measured at center -of -mass energies from root s = 4.178 to 4.278 GeV using a data sample of 7 fb(-1) collected with the BESIII detector operating at the BEPCII storage ring. The dependence of the cross section on root s shows a resonant structure with mass of (4218.5 +/- 1.6(stat) +/- 4.0(syst)) MeV/c(2) and width of (28.2 +/- 3.9(stat) +/- 1.6(syst)) MeV, respectively. This observation confirms and improves upon the result of a previous study. The angular distribution of the e(+) e(-) ->omega chi(C0) process is extracted for the first time
Study of e(+)e(-) -> omega chi(cJ) at center of mass energies from 4.21 to 4.42 Gev
No full textÇetin, Serkant Ali (Dogus Author)Based on data samples collected with the BESIII detector at the BEPCII collider at nine center of mass energies from 4.21 to 4.42 GeV, we search for the production of e(+)e(-) -> omega chi(cJ) (J = 0, 1, 2). The process e(+)e(-) -> omega chi(c0) is observed for the first time, and the Born cross sections at root s = 4.23 and 4.26 GeV are measured to be (55.4 +/- 6.0 +/- 5.9) and (23.7 +/- 5.3 +/- 3.5) pb, respectively, where the first uncertainties are statistical and the second are systematic. The omega chi(c0) signals at the other seven energies and the e(+)e(-) -> omega chi(c1) and omega chi(c2) signals are not significant, and the upper limits on the cross sections are determined. By examining the omega chi(c0) cross section as a function of center of mass energy, we find that it is inconsistent with the line shape of the Y(4260) observed in e(+)e(-) -> pi(+)pi(-) J/psi Assuming the omega chi(c0) signals come from a single resonance, we extract the mass and width of the resonance to be (4230 +/- 8 +/- 6) MeV/c(2) and (38 +/- 12 +/- 2) MeV, respectively, and the statistical significance is more than 9 sigma
Flickertail Follies - 1948 Pi Beta Phi and Alpha Tau Omega
No full textNine performers of the combined act of Pi Beta Phi and Alpha Tau Omega\u27s Prints from Currier and Ives for the 1948 Flickertail Follies. Established by the Journalism Fraternity, Sigma Delta Chi, as a campus talent and variety show, The Flickertail Follies entertained the city of Grand Forks from 1925-1962. The Follies were, however, suspended from 1931-1935 due to The Depression and from 1941-1945 for World War II. The Follies gained national attention in 1950 when it was featured in Life Magazine . The show was dropped in 1962 but was revitalized for one year in 1982.https://commons.und.edu/archive-photos/1414/thumbnail.jp
Study of e(+)e(-) -> omega chi(cJ) at Center of Mass Energies from 4.21 to 4.42 GeV
No full textBased on data samples collected with the BESIII detector at the BEPCII collider at nine center of mass energies from 4.21 to 4.42 GeV, we search for the production of e(+)e(-) -> omega chi(cJ) (J = 0, 1, 2). The process e(+)e(-) -> omega chi(c0) is observed for the first time, and the Born cross sections at root s = 4.23 and 4.26 GeV are measured to be (55.4 +/- 6.0 +/- 5.9) and (23.7 +/- 5.3 +/- 3.5) pb, respectively, where the first uncertainties are statistical and the second are systematic. The omega chi(c0) signals at the other seven energies and the e(+)e(-) -> omega chi(c1) and omega chi(c2) signals are not significant, and the upper limits on the cross sections are determined. By examining the omega chi(c0) cross section as a function of center of mass energy, we find that it is inconsistent with the line shape of the Y(4260) observed in e(+)e(-) -> pi(+)pi(-) J/psi Assuming the omega chi(c0) signals come from a single resonance, we extract the mass and width of the resonance to be (4230 +/- 8 +/- 6) MeV/c(2) and (38 +/- 12 +/- 2) MeV, respectively, and the statistical significance is more than 9 sigma
Effects of time-varying β in SNLS3 on constraining interacting dark energy models
No full textIt has been found that, for the Supernova Legacy Survey three-year (SNLS3) data, there is strong evidence for the redshift evolution of the color-luminosity parameter beta. In this paper, adopting the omega-cold-dark-matter (omega CDM) model and considering its interacting extensions (with three kinds of interaction between dark sectors), we explore the evolution of beta and its effects on parameter estimation. In addition to the SNLS3 data, we also use the latest Planck distance priors data, the galaxy clustering data extracted from sloan digital sky survey data release 7 and baryon oscillation spectroscopic survey, as well as the direct measurement of Hubble constant H-0 from the Hubble Space Telescope observation. We find that, for all the interacting dark energy (IDE) models, adding a parameter of beta can reduce chi 2 by similar to 34, indicating that a constant beta is ruled out at 5.8 sigma confidence level. Furthermore, it is found that varying beta can significantly change the fitting results of various cosmological parameters: for all the dark energy models considered in this paper, varying beta yields a larger fractional CDM densities Omega(c0) and a larger equation of state omega; on the other side, varying beta yields a smaller reduced Hubble constant h for the omega CDMmodel, but it has no impact on h for the three IDE models. This implies that there is a degeneracy between h and coupling parameter gamma. Our work shows that the evolution of beta is insensitive to the interaction between dark sectors, and then highlights the importance of considering beta is evolution in the cosmology fits.Physics, Particles & FieldsSCI(E)[email protected]
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Polarization dependence of magnetic neutron scattering
No full textThe polarization dependence of magnetic neutron scattering is shown to depend on the imaginary part of the symmetric generalized susceptibility, chi/sub s//sup ..cap alpha beta../ = /sup 1///sub 2/(chi/sup ..cap alpha beta../(Q,..omega..) + chi/sup ..beta cap alpha../(Q,..omega..), as well as on the real part of the antisymmetric susceptibility, chi/sub a//sup ..cap alpha beta../ = /sup 1///sub 2/(chi/sup ..cap alpha beta../(Q,..omega..) - chi/sup ..beta cap alpha../(Q,..omega..)). The latter term contains the spin-wave contributions to the polarization-dependent scattering, along with other effects which are a consequence of the presence of a magnetic field or a spiral structure
Exploring the evolution of color-luminosity parameter beta and its effects on parameter estimation
No full textIt has been found in previous studies that, for the Supernova Legacy Survey three-year (SNLS3) data, there is strong evidence for the redshift evolution of color-luminosity parameter beta. In this paper, using the three simplest dark energy models, i.e., the Lambda-cold-dark-matter (Lambda CDM) model, the wCDM model, and the Chevallier-Polarski-Linder model, we further explore the evolution of beta and its effects on parameter estimation. In addition to the SNLS3 data, we also take into account the Planck distance priors data of the cosmic microwave background (CMB), as well as the latest galaxy clustering (GC) data extracted from SDSS DR7 and BOSS. We find that, for all the models, adding a parameter of beta can reduce chi(2)(min) by similar to 36, indicating that beta(1) = 0 is ruled out at 6 sigma confidence levels. In other words, beta deviates from a constant at 6s confidence levels. This conclusion is insensitive to the dark energy models considered, showing the importance of considering the evolution of beta in the cosmology fits. Furthermore, it is found that varying beta can significantly change the fitting results of various cosmological parameters: using the SNLS3 data alone, varying beta yields a larger Omega(m) for the Lambda CDM model; using the SNLS3+CMB+GC data, varying beta yields a larger Omega(m) and a smaller h for all the models. Moreover, we find that these results are much closer to those given by the CMB+GC data compared to the cases of treating beta as a constant. This indicates that considering the evolution of beta is very helpful for reducing the tension between supernova and other cosmological observations.Astronomy & AstrophysicsPhysics, Particles & FieldsSCI(E)[email protected]; [email protected]; [email protected]
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