The training of trainers for legal Interpreting and Translation

This chapter addresses the person specification, core skills, training curricula and monitoring of trainers of legal interpreters and translators

Interpreting in the UK community: some reflections on public service interpreting in the UK

Starting with the question, 'why do we need professional public service interpreters?' this paper offers an overview of the present situation regarding the provision of public service interpreters in the UK to public sector clients

Chandra X-ray observation of the young stellar cluster NGC 3293 in the Carina Nebula Complex

We characterize the stellar population of the poorly explored young stellar cluster NGC 3293 at the northwestern periphery of the Carina Nebula Complex, in order to evaluate the cluster age and the mass function, and to test claims of an abnormal IMF and a deficit of M <= 2.5 M_sun stars. We performed a deep (70 ksec) X-ray observation of NGC 3293 with Chandra and detected 1026 individual X-ray point sources. We identify counterparts for 74% of the X-ray sources in deep near-infrared images. Our data clearly show that NGC 3293 hosts a large population of solar-mass stars, refuting claims of a lack of M <= 2.5 M_sun stars. The analysis of the color magnitude diagram suggests an age of ~8-10 Myr for the low-mass population of the cluster. There are at least 511 X-ray detected stars with color magnitude positions that are consistent with young stellar members within 7 arcmin of the cluster center. The number ratio of X-ray detected stars in the 1-2 M_sun range versus the M >= 5 M_sun stars (known from optical spectroscopy) is consistent with the expectation from a normal field initial mass function. Most of the early B-type stars and 20% of the later B-type stars are detected as X-ray sources. Our data shows that NGC 3293 is one of the most populous stellar clusters in the entire Carina Nebula Complex. The cluster probably harbored several O-type stars, whose supernova explosions may have had an important impact on the early evolution of the Carina Nebula Complex.Comment: accepted for Astronomy & Astrophysic

Molecular basis for modulation of the p53 target selectivity by KLF4

The tumour suppressor p53 controls transcription of various genes involved in apoptosis, cell-cycle arrest, DNA repair and metabolism. However, its DNA-recognition specificity is not nearly sufficient to explain binding to specific locations in vivo. Here, we present evidence that KLF4 increases the DNA-binding affinity of p53 through the formation of a loosely arranged ternary complex on DNA. This effect depends on the distance between the response elements of KLF4 and p53. Using nuclear magnetic resonance and fluorescence techniques, we found that the amino-terminal domain of p53 interacts with the KLF4 zinc fingers and mapped the interaction site. The strength of this interaction was increased by phosphorylation of the p53 N-terminus, particularly on residues associated with regulation of cell-cycle arrest genes. Taken together, the cooperative binding of KLF4 and p53 to DNA exemplifies a regulatory mechanism that contributes to p53 target selectivity

Reliability of GRBAS evaluation of voice quality in children who have a history of airway reconstruction surgery and how this compares to parental report of voice-related quality of life

Voice evaluation includes laryngoscopy, perceptual judgement of voice quality, evaluation of respiratory function, acoustic analysis of the voice signal and patient reported subjective impact of voice on quality of life. This is recommended in adults (Dejonkere et al 2001) and children (Cohen et al 2012). Perceptual evaluation of voice often follows the CAPE-V (ASHA 2002) or GRBAS (Hirano 1981). Children requiring laryngotracheal reconstruction (LTR) surgery tend to have this procedure during infancy, where subglottic stenosis forms following intubation in medically fragile or premature infants. Clinicians require reliable measures, particularly where there is a degree of subjectivity. Aspects of the CAPE-V show a high degree of reliability in rating of severity, pitch, breathiness and roughness (Krival et al 2007, Kelchner et al 2008). UK clinicians favour the GRBAS though there is little published information about reliability in a paediatric population. Comparison of clinician perceptual evaluation with patient report shows weak agreement in adults (Karnell et al 2006) reinforcing the need for both measurements. The extent to which the same is the case in children needs further exploration

The Detonation Mechanism of the Pulsationally-Assisted Gravitationally-Confined Detonation Model of Type Ia Supernovae

We describe the detonation mechanism comprising the "Pulsationally Assisted" Gravitationally Confined Detonation (GCD) model of Type Ia supernovae SNe Ia. This model is analogous to the previous GCD model reported in Jordan et al.(2008); however, the chosen initial conditions produce a substantively different detonation mechanism, resulting from a larger energy release during the deflagration phase. The resulting final kinetic energy and nickel-56 yields conform better to observational values than is the case for the "classical" GCD models. In the present class of models, the ignition of a deflagration phase leads to a rising, burning plume of ash. The ash breaks out of the surface of the white dwarf, flows laterally around the star, and converges on the collision region at the antipodal point from where it broke out. The amount of energy released during the deflagration phase is enough to cause the star to rapidly expand, so that when the ash reaches the antipodal point, the surface density is too low to initiate a detonation. Instead, as the ash flows into the collision region (while mixing with surface fuel), the star reaches its maximally expanded state and then contracts. The stellar contraction acts to increase the density of the star, including the density in the collision region. This both raises the temperature and density of the fuel-ash mixture in the collision region and ultimately leads to thermodynamic conditions that are necessary for the Zel'dovich gradient mechanism to produce a detonation. We demonstrate feasibility of this scenario with three 3-dimensional (3D), full star simulations of this model using the FLASH code. We characterized the simulations by the energy released during the deflagration phase, which ranged from 38% to 78% of the white dwarf's binding energy. We show that the necessary conditions for detonation are achieved in all three of the models.Comment: 22 pages, 8 figures; Ap

Classical Novae as a Probe of the Cataclysmic Variable Population

Classical Novae (CNe) are the brightest manifestation of mass transfer onto a white dwarf in a cataclysmic variable (CV). As such, they are probes of the mass transfer rate, Mdot, and WD mass, Mwd, in these interacting binaries. Our calculations of the dependence of the CN ignition mass, Mign, on Mdot and Mwd yields the recurrence times of these explosions. We show that the observed CNe orbital period distribution is consistent with the interrupted magnetic braking evolutionary scenario, where at orbital periods Porb > 3 hr mass transfer is driven by angular momentum loss via a wind from the companion star and at Porb < 3 hr by gravitational radiation. About 50% of CNe occur in binaries accreting at Mdot ~= 10^{-9} Msun/yr with Porb = 3-4 hr, with the remaining 50% split evenly between Porb longer (higher Mdot) and shorter (lower Mdot) than this. This resolution of the relative contribution to the CN rate from different CVs tells us that 3(9)x10^5 CVs with WD mass 1.0(0.6)Msun are needed to produce one CN per year. Using the K-band specific CN rate measured in external galaxies, we find a CV birthrate of 2(4)x10^{-4}/yr per 10^{10}Lsun,K, very similar to the luminosity specific Type Ia supernova rate in elliptical galaxies. Likewise, we predict that there should be 60-180 CVs for every 10^6Lsun,K in an old stellar population, similar to the number of X-ray identified CVs in the globular cluster 47 Tuc, showing no overabundance relative to the field. Using a two-component steady state model of CV evolution we show that the fraction of CVs which are magnetic (22%) implies a birthrate of 8% relative to non-magnetic CVs, similar to the fraction of strongly magnetic field WDs. (abridged)Comment: 6 pages, 2 figures, Accepted to the Astrophysical Journa

Measuring White Dwarf Accretion Rates via their Effective Temperatures

Our previous theoretical study of the impact of an accreting envelope on the thermal state of an underlying white dwarf (WD) has yielded equilibrium core temperatures, classical nova ignition masses and thermal luminosities for WDs accreting at time averaged rates of = 10^-11 - 10^-8 Msun/yr. These 's are appropriate to WDs in cataclysmic variables (CVs) of P_orb <~ 7 hr, many of which accrete sporadically as Dwarf Novae. Approximately thirty nonmagnetic Dwarf Novae have been observed in quiescence, when the accretion rate is low enough for spectral detection of the WD photosphere, and a measurement of T_eff. We use our theoretical work to translate the measured T_eff's into local time-averaged accretion rates, confirming the factor of ten drop in predicted for CV's as they transit the period gap. For DN below the period gap, we show that if is that given by gravitational radiation losses alone, then the WD masses are > 0.8 Msun. An alternative conclusion is that the masses are closer to 0.6 Msun and is 3-4 times larger than that expected from gravitational radiation losses. In either case, it is very plausible that a subset of CVs with P_orb < 2 hours will have T_eff's low enough for them to become non-radial pulsators, as discovered by van Zyl and collaborators in GW Lib.Comment: 4 pages, 3 figures; uses emulateapj; Accepted by the Astrophysical Journal Letter