Rubin-LSST

Abstract:

We report the observation of Bs0- B̄s0 oscillations from a time-dependent measurement of the Bs0-B̄s0 oscillation frequency Δms. Using a data sample of 1 fb-1 of pp collisions at √ = 1.96 TeV collected with the CDF II detector at the Fermilab Tevatron, we find signals of 5600 fully reconstructed hadronic B s decays, 3100 partially reconstructed hadronic Bs decays, and 61500 partially reconstructed semileptonic Bs decays. We measure the probability as a function of proper decay time that the Bs decays with the same, or opposite, flavor as the flavor at production, and we find a signal for Bs0-B̄s0 oscillations. The probability that random fluctuations could produce a comparable signal is 8 × 10-8, which exceeds 5σ significance. We measure Δms = 17.77 ± 0.10(stat) ± 0.07(syst) ps-1 and extract |Vtd/Vts| = 0.2060 ± 0.0007(Δms)-0.0060+0.0081 (Δmd + theor). © 2006 The American Physical Society.

Abstract:

We present two-degree field spectroscopic observations of a sample of 96 A-type stars selected from the Sloan Digital Sky Survey Data Release 3 (SDSS DR3). Our aim is to identify blue horizontal branch (BHB) stars in order to measure the kinematic properties of the tidal tails of the Sagittarius dwarf spheroidal galaxy. We confine our attention to the 44 classifiable stars with spectra of signal-to-noise ratio > 15 Å-1. Classification produces a sample of 29 BHB stars at distances of 5-47 kpc from the Sun. We split our sample into three bins based on their distance. We find 10 of the 12 stars at 14-25 kpc appear to have coherent, smoothly varying radial velocities which are plausibly associated with old debris in the Sagittarius tidal stream. Further observations along the orbit and at greater distances are required to trace the full extent of this structure on the sky. Three of our BHB stars in the direction of the globular cluster Palomar (Pal) 5 appear to be in an overdensity but are in the foreground of Pal 5. More observations are required around this overdensity to establish any relation to Pal 5 and/or the Sgr stream. We emphasize observations of BHB stars have unlimited potential for providing accurate velocity and distance information in old distant halo streams and globular clusters alike. The next-generation multi-object spectrographs provide an excellent opportunity to accurately trace the full extent of such structures. © 2006 RAS.

Abstract:

We seek to understand whether the stellar populations of galactic bulges show evidence of secular evolution triggered by the presence of the disc. For this purpose, we re-analyse the sample of Proctor and Sansom, deriving stellar population ages and element abundances from absorption-line indices as functions of central velocity dispersion and Hubble type. We obtain consistent constraints on ages from the three Balmer-line indices Hβ, Hγ and Hδ, based on stellar population models that take the abundance ratio effects on these indices into account. Emission-line contamination turns out to be a critical aspect, which favours the use of the higher order Balmer-line indices. Our derived ages are consistent with those of Proctor and Sansom based on a completely different method. In agreement with other studies in the literature, we find that bulges have relatively low luminosity weighted ages, the lowest age derived being 1.3 Gyr. Hence, bulges are not generally old, but actually rejuvenated systems. We discuss evidence that this might be true also for the bulge of the Milky Way. The data reveal clear correlations of all three parameters luminosity weighted age, total metallicity and α/Fe ratio with central velocity dispersion. The smallest bulges are the youngest with the lowest α/Fe ratios owing to late Fe enrichment from Type Ia supernovae. Using models combining recent minor star formation with a base old population, we show that the smallest bulges must have experienced significant star formation events involving 10-30 per cent of their total mass in the past 1-2 Gyr. No significant correlations of the stellar population parameters with Hubble type are found. We show that the above relationships with σ coincide perfectly with those of early-type galaxies. In other words, bulges are typically younger, metal poorer and less α/Fe enhanced than early-type galaxies because of their smaller masses. At a given velocity dispersion, bulges and elliptical galaxies are indistinguishable as far as their stellar populations are concerned. These results favour an inside-out formation scenario and indicate that the discs in spiral galaxies of Hubble types Sbc and earlier cannot have a significant influence on the evolution of the stellar populations in the bulge component. The phenomenon of pseudo-bulge formation must be restricted to spirals of types later than Sbc. © 2005 RAS.

Abstract:

We report the results of a search for a charged Higgs boson in the decays of top quarks produced in pp̄ collisions at a center-of-mass energy of 1.96 TeV. We use a data sample corresponding to an integrated luminosity of 193pb-1 collected by the upgraded Collider Detector at Fermilab. No evidence for charged Higgs production is found, allowing 95% C.L. upper limits to be placed on BR(t→H+b) for different charged Higgs decay scenarios. In addition, we present in the minimal supersymmetric standard model (mH±,tan β) plane the first exclusion regions with radiative and Yukawa coupling corrections. © 2006 The American Physical Society.

Abstract:

We search for excited and exotic muon states * using an integrated luminosity of 371pb-1 of pp collision data at s=1.96TeV. We search for associated production of * followed by the decay *. We compare the data to model predictions as a function of the mass of the excited muon M *, the compositeness energy scale , and the gauge coupling factor f. No signal above the standard model expectation is observed. We exclude 107

More details from the publisher