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Ian M. Bassett,Shichun Lun,William R. Bishai,Haidan Guo,Joanna R. Kirman,Mudassar Altaf,Ronan F. O’Toole 한국미생물학회 2013 The journal of microbiology Vol.51 No.5
Many whole cell screens of chemical libraries currently in use are based on inhibition of bacterial growth. The goal of this study was to develop a chemical library screening model that enabled detection of compounds that are active against drug-tolerant non-growing cultures of Mycobacterium tuberculosis. An in vitro model of low metabolically active mycobacteria was established with 8 and 30 day old cultures of M. smegmatis and M. tuberculosis, respectively. Reduction of resazurin was used as a measure of viability and the assay was applied in screens of chemical libraries for bactericidal compounds. The model provided cells that were phenotypically-resilient to killing by first and second-line clinical drugs including rifampicin. Screening against chemical libraries identified proteasome inhibitors, NSC310551 and NSC321206, and a structurally-related series of thiosemicarbazones,as having potent killing activity towards aged cultures. The inhibitors were confirmed as active against virulent M. tuberculosis strains including multi- and extensively-drug resistant clinical isolates. Our library screen enabled detection of compounds with a potent level of bactericidal activity towards phenotypically drug-tolerant cultures of M. tuberculosis.
DARK ENERGY REFLECTIONS IN THE REDSHIFT-SPACE QUADRUPOLE
NISHIOKA HIROAKI,YAMAMOTO KAZUHIRO,BASSETT BRUCE A. The Korean Astronomical Society 2005 Journal of The Korean Astronomical Society Vol.38 No.2
We show that next-generation galaxy surveys such as KAOS (the Kilo-Aperture Optical Spectro-graph)will constrain dark energy even if the baryon oscillations are missing from the monopole power spectrum and the bias is scale- and time-dependent KAOS will accurately measure the quadrupole power spectrum which gives the leading anisotropies in the power spectrum in redshift space due to peculiar velocities, the finger of God effect, as well as the Alcock-Paczynski effect. The combination of monopole and quadrupole power spectra powerfully breaks the degeneracy between the bias parameters and dark energy and, in the complete absence of baryon oscillations ($\Omega$b = 0), leads to a roughly $500\%$ improvement in constraints on dark energy compared with the monopole spectrum alone. As a result, for KAOS the worst case with no oscillations has dark energy errors only mildly degraded relative to the ideal case, providing insurance on the robustness of KAOS constraints on dark energy. We show that nonlinear effects are crucial in correctly evaluating the quadrupole and significantly improving the constraints on dark energy when we allow for multi-parameter scale-dependent bias.
THE EFFECT OF HOST GALAXIES ON TYPE Ia SUPERNOVAE IN THE SDSS-II SUPERNOVA SURVEY
Lampeitl, Hubert,Smith, Mathew,Nichol, Robert C.,Bassett, Bruce,Cinabro, David,Dilday, Benjamin,Foley, Ryan J.,Frieman, Joshua A.,Garnavich, Peter M.,Goobar, Ariel,Im, Myungshin,Jha, Saurabh W.,Marrin IOP Publishing 2010 The Astrophysical journal Vol.722 No.1
( Tarek Boutefnouchet ),( Christopher Downham ),( James Bassett ),( Peter Thompson ),( Andrew Sprowson ) 대한슬관절학회 2016 대한슬관절학회지 Vol.28 No.2
A systematic review of the literature was undertaken to evaluate the efficacy of medial patellofemoral ligament (MPFL) reconstruction combined with tibial tuberosity transfer (TTT) in the treatment of patellofemoral instability. Using PRISMA (Preferred Reporting Items for Systematic Reviews and Meta-Analyses) guidelines, a systematic search was carried out to identify and review the published literature pertinent to MFPL reconstruction combined with TTT. Relevant studies were critically appraised with narrative data synthesis. Studies that met the eligibility criteria were suitable for appraisal and consisted of case series and therapeutic series (levels IV & III). All studies had inherent variations in outcomes reporting and limited follow-up. Combined treatment offers restoration of normal anatomy, thus adding clinical value to the currently recommended anatomic approach to MPFL reconstruction. Nevertheless, the current body of evidence does not determine the threshold at which patellofemoral axis requires the need for adjunctive distal realignment as opposed to MPFL reconstruction alone. This review highlighted numerous recurring limitations in the conduct and presentation of the studies, which inadvertently mitigated the interpretation of their results. Future priority should be awarded to larger randomised controlled trials utilising validated patient reported outcome measures.
Macaulay, E,Nichol, R C,Bacon, D,Brout, D,Davis, T M,Zhang, B,Bassett, B A,Scolnic, D,Mö,ller, A,D’Andrea, C B,Hinton, S R,Kessler, R,Kim, A G,Lasker, J,Lidman, C,Sako, M,Smith, M,Sullivan, M,Abbo Oxford University Press 2019 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.486 No.2
<B>ABSTRACT</B><P>We present an improved measurement of the Hubble constant (H0) using the ‘inverse distance ladder’ method, which adds the information from 207 Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) at redshift 0.018 < z < 0.85 to existing distance measurements of 122 low-redshift (z < 0.07) SNe Ia (Low-z) and measurements of Baryon Acoustic Oscillations (BAOs). Whereas traditional measurements of H0 with SNe Ia use a distance ladder of parallax and Cepheid variable stars, the inverse distance ladder relies on absolute distance measurements from the BAOs to calibrate the intrinsic magnitude of the SNe Ia. We find H0 = 67.8 ± 1.3 km s−1 Mpc−1 (statistical and systematic uncertainties, 68 per cent confidence). Our measurement makes minimal assumptions about the underlying cosmological model, and our analysis was blinded to reduce confirmation bias. We examine possible systematic uncertainties and all are below the statistical uncertainties. Our H0 value is consistent with estimates derived from the Cosmic Microwave Background assuming a ΛCDM universe.</P>
The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters
Brough, Sarah,van de Sande, Jesse,Owers, Matt S.,d’Eugenio, Francesco,Sharp, Rob,Cortese, Luca,Scott, Nicholas,Croom, Scott M.,Bassett, Rob,Bekki, Kenji,Bland-Hawthorn, Joss,Bryant, Julia J.,Davies, R American Astronomical Society 2017 The Astrophysical journal Vol.844 No.1
<P>We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral-field spectrograph Galaxy Survey. The clusters cover a mass range of 14.2 < log(M-200/M-circle dot) < 15.2 and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses 10.0 < log(M-*/M-circle dot) <= 11.7 within 1 R-200 of the cluster centers. We calculate the spin parameter, lambda(R), and use this to classify the kinematic morphology of the galaxies as fast or slow rotators (SRs). The total fraction of SRs in the ETG population is F-SR = 0.14 +/- 0.02 and does not depend on host cluster mass. Across the eight clusters, the fraction of SRs increases with increasing local overdensity. We also find that the slow-rotator fraction increases at small clustercentric radii (R-cl < 0.3 R-200), and note that there is also an increase in the slow-rotator fraction at R-cl similar to 0.6 R-200. The SRs at these larger radii reside in the cluster substructure. We find that the strongest increase in the slow-rotator fraction occurs with increasing stellar mass. After accounting for the strong correlation with stellar mass, we find no significant relationship between spin parameter and local overdensity in the cluster environment. We conclude that the primary driver for the kinematic morphology-density relationship in galaxy clusters is the changing distribution of galaxy stellar mass with the local environment. The presence of SRs in the substructure suggests that the cluster kinematic morphology-density relationship is a result of mass segregation of slow-rotating galaxies forming in groups that later merge with clusters and sink to the cluster center via dynamical friction.</P>