Rubin-LSST

Abstract:

We present the report of the hadronic working group of the BOOST2010 workshop held at the University of Oxford in June 2010. The first part contains a review of the potential of hadronic decays of highly boosted particles as an aid for discovery at the LHC and a discussion of the status of tools developed to meet the challenge of reconstructing and isolating these topologies. In the second part, we present new results comparing the performance of jet grooming techniques and top tagging algorithms on a common set of benchmark channels. We also study the sensitivity of jet substructure observables to the uncertainties in Monte Carlo predictions.

Abstract:

We perform numerical simulations of large scale structure evolution in an inhomogeneous Lemaître-Tolman-Bondi (LTB) model of the Universe. We follow the gravitational collapse of a large underdense region (a void) in an otherwise flat matter-dominated Einstein–de Sitter model. We observe how the (background) density contrast at the center of the void grows to be of order one, and show that the density and velocity profiles follow the exact nonlinear LTB solution to the full Einstein equations for all but the most extreme voids. This result seems to contradict previous claims that fully relativistic codes are needed to properly handle the nonlinear evolution of large scale structures, and that local Newtonian dynamics with an explicit expansion term is not adequate. We also find that the (local) matter density contrast grows with the scale factor in a way analogous to that of an open universe with a value of the matter density Ω M ( r ) corresponding to the appropriate location within the void.

Abstract:

We report the first determination of the relative strong-phase difference between D0→KS,L0K+K- and D⊃̄0→KS, L0K+K-. In addition, we present updated measurements of the relative strong-phase difference between D0→KS, L0π+π- and D⊃̄0→KS,L0π +π-. Both measurements exploit the quantum coherence between a pair of D0 and D⊃̄0 mesons produced from ψ(3770) decays. The strong-phase differences measured are important for determining the Cabibbo-Kobayashi-Maskawa angle γ/Φ3 in B -→K-D⊃0 decays, where D⊃0 is a D0 or D⊃̄0 meson decaying to KS0h+h- (h=π, K), in a manner independent of the model assumed to describe the D0→KS0h +h- decay. Using our results, the uncertainty in γ/Φ3 due to the error on the strong-phase difference is expected to be between 1.7° and 3.9° for an analysis using B -→K-D⊃0, D⊃0→KS0π+π - decays, and between 3.2° and 3.9° for an analysis based on B-→K-D⊃0, D⊃0→KS0K+K - decays. A measurement is also presented of the CP-odd fraction, F-, of the decay D0→KS0K+K- in the region of the Φ→K+K- resonance. We find that in a region within 0.01GeV2/c4 of the nominal Φ mass squared F->0.91 at the 90% confidence level. © 2010 The American Physical Society.

Abstract:

We report a detailed spectral analysis of the population of low-massX-ray binaries (LMXBs) detected in the elliptical galaxy NGC 4278 with Chandra. Seven luminous sources were studied individually, four in globular clusters (GCs) and three in the stellar field. The range of (0.3-8 keV) LX for these sources is ∼(3-8) × 1038 erg s-1, suggesting that they may be black hole binaries (BHBs). Fitting the data with either single thermal accretion disk or power-law (PO) models results in best-fit temperatures of ∼0.7-1.7 keV and Λ ∼ 1.2-2.0, consistent with those measured in Galactic BHBs. Comparison of our results with simulations allows us to discriminate between disk and power-lawdominated emission, pointing to spectral/luminosity variability, reminiscent of Galactic BHBs. The BH masses derived from a comparison of our spectral results with the LX ≥ T in4 relation of Galactic BHBs are in the 5-15M⊙ range, as observed in the Milky Way. The analysis of joint spectra of sources selected in three luminosity ranges (LX ≥ 1.5 × 1038 erg s-1, 6 × 1037 erg s-1 ≤ LX < 1.5 × 1038 erg s-1, and LX < 6 × 1037 erg s-1) suggests that while the high-luminosity sources have prominent thermal disk emission components, power-law components are likely to be important in the mid- and low-luminosity spectra. Comparing low-luminosity average spectra, we find a relatively larger NH in the GC spectrum; we speculate that this may point to either a metallicity effect or to intrinsic physical differences between field and GC accreting binaries. Analysis of average sample properties uncovers a previously unreported L X-RG correlation (where RG is the galactocentric radius) in the GC-LMXB sample, implying richer LMXB populations in more central GCs. No such trend is seen in the field LMXB sample. We can exclude that the GC LX-RG correlation is the by-product of a luminosity effect and suggest that it may be related to the presence of more compact GCs at smaller galactocentric radii, fostering more efficient binary formation. © 2010. The American Astronomical Society. All rights reserved.