Testing hydrodynamics schemes in galaxy disc simulations

We examine how three fundamentally different numerical hydrodynamics codes follow the evolution of an isothermal galactic disc with an external spiral potential. We compare an adaptive mesh refinement code (RAMSES), a smoothed particle hydrodynamics code (SPHNG), and a volume-discretised meshless code (GIZMO). Using standard refinement criteria, we find that RAMSES produces a disc that is less vertically concentrated and does not reach such high densities as the SPHNG or gizmo runs. The gas surface density in the spiral arms increases at a lower rate for the RAMSES simulations compared to the other codes. There is also a greater degree of substructure in the SPHNG and GIZMOruns and secondary spiral arms are more pronounced. By resolving the Jeans’ length with a greater number of grid cells we achieve more similar results to the Lagrangian codes used in this study. Other alterations to the refinement scheme (adding extra levels of refinement and refining based on local density gradients) are less successful in reducing the disparity between RAMSES and SPHNG/GIZMO. Although more similar, SPHNG displays different density distributions and vertical mass profiles to all modes of gizmo (including the smoothed particle hydrodynamics version). This suggests differences also arise which are not intrinsic to the particular method but rather due to its implementation. The discrepancies between codes (in particular, the densities reached in the spiral arms) could potentially result in differences in the locations and timescales for gravitational collapse, and therefore impact star formation activity in more complex galaxy disc simulations

Modular Interoperable Synthetic Environment: Final Report

Report on Modular interoperable synthetic environment which is an attempt to research and address difficulties with interoperablility among systems which incorporate varying levels of fidelity and diverse communications protocols in the absence of a definitive and comprehensive set of standards

The morphology of the Milky Way - II. Reconstructing CO maps from disc galaxies with live stellar distributions

The arm structure of the Milky Way remains somewhat of an unknown, with observational studies hindered by our location within the Galactic disc. In the work presented here we use smoothed particle hydrodynamics (SPH) and radiative transfer to create synthetic longitude-velocity observations. Our aim is to reverse-engineer a top down map of the Galaxy by comparing synthetic longitude-velocity maps to those observed. We set up a system of N-body particles to represent the disc and bulge, allowing for dynamic creation of spiral features. Interstellar gas, and the molecular content, is evolved alongside the stellar system. A 3D-radiative transfer code is then used to compare the models to observational data. The resulting models display arm features that are a good reproduction of many of the observed emission structures of the Milky Way. These arms however are dynamic and transient, allowing for a wide range of morphologies not possible with standard density wave theory. The best fitting models are a much better match than previous work using fixed potentials. They favour a 4-armed model with a pitch angle of approximately 20 degrees, though with a pattern speed that decreases with increasing Galactic radius. Inner bars are lacking however, which appear required to fully reproduce the central molecular zone.Comment: 16 pages, 15 figures, accepted by MNRA

Bridging the phenotypic gap: Real-time assessment of mitochondrial function and metabolism of the nematode Caenorhabditis elegans

Peer reviewedPublisher PD

An Inversion Disrupting FAM134B Is Associated with Sensory Neuropathy in the Border Collie Dog Breed

Sensory neuropathy in the Border Collie is a severe neurological disorder caused by the degeneration of sensory and, to a lesser extent, motor nerve cells with clinical signs starting between 2 and 7 months of age. Using a genome-wide association study approach with three cases and 170 breed matched controls, a suggestive locus for sensory neuropathy was identified that was followed up using a genome sequencing approach. An inversion disrupting the candidate gene FAM134B was identified. Genotyping of additional cases and controls and RNAseq analysis provided strong evidence that the inversion is causal. Evidence of cryptic splicing resulting in novel exon transcription for FAM134B was identified by RNAseq experiments. This investigation demonstrates the identification of a novel sensory neuropathy associated mutation, by mapping using a minimal set of cases and subsequent genome sequencing. Through mutation screening, it should be possible to reduce the frequency of or completely eliminate this debilitating condition from the Border Collie breed population

Agouti C57BL/6N embryonic stem cells for mouse genetic resources.

We report the characterization of a highly germline competent C57BL/6N mouse embryonic stem cell line, JM8. To simplify breeding schemes, the dominant agouti coat color gene was restored in JM8 cells by targeted repair of the C57BL/6 nonagouti mutation. These cells provide a robust foundation for large-scale mouse knockout programs that aim to provide a public resource of targeted mutations in the C57BL/6 genetic background

The Influence of Start Position, Initial Step Type, and Usage of a Focal Point on Sprinting Performance

International Journal of Exercise Science 6(4) : 320-327, 2013. For many athletes, sprinting acceleration is vital to sport performance. The purpose of this study was to observe the influences of starting position, type of initial step taken, and a focal point on sprinting velocity, stride length, and acceleration over a 9.1 m distance. Two trials of four conditions were video recorded in which subjects had no focal point (n = 10) or a lateral focal point (n = 9). The four conditions were: forwards (control), backwards, 90° left (90°L), and 90° right (90°R). Lower velocities (p \u3e 0.05) were observed with focal point usage from the 90°R and 90°L starting positions. Four initial steps were observed during the forwards, 90°L, and 90°R conditions: backwards step, anterior tilt with forward step, pivot-crossover step, and lateral side step. The use of a backwards step resulted in an increased velocity (+0.80 m·s-1, p \u3c 0.01) for the 90° turn trials and increased acceleration (+ 0.37 m·s-2,p \u3c 0.01). Our results indicate that looking at a target can cause a decline in sprint velocity and acceleration over a short distance. Moreover, utilizing a backwards step to initiate a 90° turn may generate more power and force, increasing their velocity for short sprints. We recommend training athletes with a target or focal points to help combat the reduced speed and initiate movement with initial backwards step

Simulations of the flocculent spiral M33: what drives the spiral structure?

We perform simulations of isolated galaxies in order to investigate the likely origin of the spiral structure in M33. In our models, we find that gravitational instabilities in the stars and gas are able to reproduce the observed spiral pattern and velocity field of M33, as seen in HI, and no interaction is required. We also find that the optimum models have high levels of stellar feedback which create large holes similar to those observed in M33, whilst lower levels of feedback tend to produce a large amount of small scale structure, and undisturbed long filaments of high surface density gas, hardly detected in the M33 disc. The gas component appears to have a significant role in producing the structure, so if there is little feedback, both the gas and stars organise into clear spiral arms, likely due to a lower combined $Q$ (using gas and stars), and the ready ability of cold gas to undergo spiral shocks. By contrast models with higher feedback have weaker spiral structure, especially in the stellar component, compared to grand design galaxies. We did not see a large difference in the behaviour of $Q_{stars}$ with most of these models, however, because $Q_{stars}$ stayed relatively constant unless the disc was more strongly unstable. Our models suggest that although the stars produce some underlying spiral structure, this is relatively weak, and the gas physics has a considerable role in producing the large scale structure of the ISM in flocculent spirals.Comment: 17 pages, 17 figures, accepted for publication in MNRA

Incidence of proteinuria in type 2 diabetes mellitus in the Pima Indians

Incidence of proteinuria in type 2 diabetes mellitus in the Pima Indians. Little is known of the natural history of nephropathy in type 2 (non-insulin-dependent) diabetes, yet type 2 diabetes is a major cause of end-stage renal disease in the United States. The incidence rate of heavy proteinuria was determined in Pima Indians participating in a longitudinal population study of diabetes and its complications. Heavy proteinuria was defined by a urine protein (g/liter) to urine creatinine (g/liter) ratio ≥ 1.0 (≥ 113mg protein/mmol creatinine), a level which corresponds to a urine protein excretion rate of about 1 g/day. The incidence rates of proteinuria in diabetic Pimas were 4, 12, 37, and 106 cases/1,000 person-years at risk in the periods 0 to 5, 5 to 10, 10 to 15, and 15 to 20 years after the diagnosis of diabetes. The cumulative incidence rates were 2%, 8%, 23%, and 50% at 5, 10, 15, and 20 years, respectively. The duration of diabetes, severity of diabetes as determined by the degree of hyperglycemia and type of treatment, and blood pressure were risk factors for proteinuria. The presence of heavy proteinuria was strongly associated with the development of renal insufficiency, defined by serum creatinine ≥ 2.0 mg/dl (≥ 177 µmol/liter). The incidence of proteinuria in type 2 diabetes in Pima Indians was as high as that reported in type 1 diabetes in other populations and represents a frequent, serious complication of the disease