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The SAMI Galaxy Survey: Kinematic Alignments of Early-type Galaxies in A119 and A168
Jeong, Hyunjin,Kim, Suk,Owers, Matt S.,Joo, Seok-Joo,Kim, Hak-Sub,Lee, Woong,Lee, Youngdae,Sande, Jesse van de,Lee, Jaehyun,Yi, Sukyoung K.,Croom, Scott M.,Bryant, Julia J.,Rey, Soo-Chang,Brough, Sara American Astronomical Society 2019 The Astrophysical journal Vol.875 No.1
Endoscopic Evaluation of Biliary Strictures: Current and Emerging Techniques
Roy Huynh,Corinne Owers,Christopher Pinto,Thuy-My Nguyen,Titus Kwok 대한소화기내시경학회 2021 Clinical Endoscopy Vol.54 No.6
The diagnosis of biliary strictures in clinical practice can be challenging. Discriminating between benign and malignant biliarystrictures is important to prevent the morbidity and mortality associated with incorrect diagnoses. Missing a malignant biliarystricture may delay surgery, resulting in poor prognostic outcomes. Conversely, it has been demonstrated that approximately20% of patients who undergo surgery for suspected biliary malignancies have a benign etiology on histopathology. Traditionaltissue sampling using endoscopic retrograde cholangiography does not always produce a definitive diagnosis, with a considerableproportion of cases remaining as indeterminate biliary strictures. Recent advances in endoscopic techniques have the potential toimprove the diagnostic and prognostic accuracy of biliary strictures.
Fabrication, microstructure and properties of Fe-TiC ceramic-metal composites
I. W. M. Brown,W. R. Owers 한국물리학회 2004 Current Applied Physics Vol.4 No.2-4
Ceramic–metal composites based on the Fe–TiC system can be synthesised by reduction of the mineral ilmenite (FeTiO3) with carbon in flowing argon or under vacuum in the temperature range 1100–1400 C. The ratio of Fe:TiC can be controlled through adjustment of the reactant materials, as can the addition of alloying metals such as Co, Cr or Ni. Dense bodies formed by sintering Fe–TiC powders displaya microstructure of uniformlydispersed TiC grains in a continuous metal matrix. The grain size of the TiC can be controlled between 1 and 20 lm byvary ing the heat treatment schedules. Hardness values of 14 GPa can be achieved through pressureless sintering of unalloyed Fe:3TiC bodies. Technologies have been developed for fabricating a range of compositions from 6 wt% to over 80 wt% TiC in iron alloymatrices, leading to broad suite of potential industrial applications as wear parts or cutting ools.
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>