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ObjectivesColorectal polyp cancers present clinicians with a treatment dilemma. Decisions regarding whether to offer segmental resection or endoscopic surveillance are often taken without reference to good quality evidence. The aim of this study was to develop a treatment algorithm for patients with screen-detected polyp cancers.DesignThis national cohort study included all patients with a polyp cancer identified through the Scottish Bowel Screening Programme between 2000 and 2012. Multivariate regression analysis was used to assess the impact of clinical, endoscopic and pathological variables on the rate of adverse events (residual tumour in patients undergoing segmental resection or cancer-related death or disease recurrence in any patient). These data were used to develop a clinically relevant treatment algorithm.Results485 patients with polyp cancers were included. 186/485 (38%) underwent segmental resection and residual tumour was identified in 41/186 (22%). The only factor associated with an increased risk of residual tumour in the bowel wall was incomplete excision of the original polyp (OR 5.61, p=0.001), while only lymphovascular invasion was associated with an increased risk of lymph node metastases (OR 5.95, p=0.002). When patients undergoing segmental resection or endoscopic surveillance were considered together, the risk of adverse events was significantly higher in patients with incomplete excision (OR 10.23, p<0.001) or lymphovascular invasion (OR 2.65, p=0.023).ConclusionA policy of surveillance is adequate for the majority of patients with screen-detected colorectal polyp cancers. Consideration of segmental resection should be reserved for those with incomplete excision or evidence of lymphovascular invasion.

We present a detailed analysis of Jupiter's X-ray (0.2-10 keV) auroral emissions as observed over two XMM-Newtonrevolutions in Nov. 2003 and compare it with that of an earlier observation in Apr. 2003. We discover the existence of an electron bremsstrahlung component in the aurorae, which accounts for essentially all the X-ray flux above 2 keV: its presence had been predicted but never detected for lack of sensitivity of previous X-ray missions. This bremsstrahlung component varied significantly in strength and spectral shape over the 3.5 days covered by the Nov. 2003 observation, displaying substantial hardening of the spectrum with increasing flux. This variability may be linked to the strong solar activity taking place at the time, and may be induced by changes in the acceleration mechanisms inside Jupiter's magnetosphere. As in Apr. 2003, the auroral spectra below 2 keV are best fitted by a superposition of line emission most likely originating from ion charge exchange, with OVII playing the dominant role. We still cannot resolve conclusively the ion species responsible for the lowest energy lines (around 0.3 keV), so the question of the origin of the ions (magnetospheric or solar wind) is still open. It is conceivable that both scenarios play a role in what is certainly a very complex planetary structure. High resolution spectra of the whole planet obtained with the XMM-NewtonReflection Grating Spectrometer in the range 0.5-1 keV clearly separate emission lines (mostly of iron) originating at low latitudes on Jupiter from the auroral lines due to oxygen. These are shown to possess very broad wings which imply velocities of ~5000 km s$^{\rm -1}$. Such speeds are consistent with the energies at which precipitating and charge exchanging oxygen ions are expected to be accelerated in Jupiter's magnetosphere. Overall we find good agreement between our measurements and the predictions of recently developed models of Jupiter's auroral processes.

ROSATobservations found no convincing evidence for X-ray sources located in local dwarf spheroidal galaxies (dSph). Now with more sensitive instruments on board Chandraand XMM-Newtonwe can reach fainter luminosity levels. We report on an observation of the Sagittarius (Sgr) dSph made using Chandraand an observation of the Carina (Car) dSph made using XMM-Newton. Our observations are sensitive to sources with X-ray luminosities in the 0.1–10 keV band of ~$1\times10^{32}$erg s-1and 3$\times10^{34}$erg s-1for the Sgr and Car fields respectively. We have identified a total of 80 sources in the Sgr field and 53 sources in the Car field. Although the source numbers are roughly consistent with the expected number of background AGN, we found a small fraction of X-ray sources which were soft and could be located in the host dSph. Follow-up optical/IR observations may help to identify their optical counterparts and hence determine their nature.

We present the results of XMM-Newtonobservations of two AM CVn systems – V396 Hya and SDSS J1240-01. Both systems are detected in X-rays and in the UV: neither shows coherent variability in their light curves. We compare the rms variability of the X-ray and UV power spectra of these sources with other AM CVn systems. Apart from ES Cet, AM CVn sources are not strongly variable in X-rays, while in the UV the degree of variability is related to the systems apparent brightness. The X-ray spectra of V396 Hya and SDSS J1240-01 show highly non-solar abundances, requiring enhanced nitrogen to obtain good fits. We compare the UV and X-ray luminosities for 7 AM CVn systems using recent distances. We find that the X-ray luminosity is not strongly dependent upon orbital period. However, the UV luminosity is highly correlated with orbital period with the UV luminosity decreasing with increasing orbital period. We expect that this is due to the accretion disk making an increasingly strong contribution to the UV emission at shorter periods. The implied luminosities are in remarkably good agreement with predictions.

We have carried out a Chandraobservation of the globular cluster M 54. We detected 7 sources located within the half-mass radius of M 54, at a flux limit of 1.5 $\times$10-15erg s-1cm-2in the 0.3-8 keV energy band. The spatial distribution and the colour/spectral properties of the 7 sources suggest that they are likely to be cataclysmic variables or LMXBs in the globular cluster. M 54 shows the largest number of X-ray sources with luminosities greater than 1032erg s-1compared to other globular clusters observed using Chandraand XMM-Newton. We searched for a correlation between the number of sources above this luminosity level with globular cluster parameters. We found evidence that the number of sources peaks at a King concentration parameter c~ 1.7–1.9, with globular clusters which are core-collapsed or have low-c values having a smaller number of sources. We speculate on possible reasons for this.

Field-channelled accretion flows occur in a variety of astrophysical objects, including T Tauri stars, magnetic cataclysmic variables and X-ray pulsars. We consider a curvilinear coordinate system and derive a general hydrodynamic formulation for accretion onto stellar objects confined by a stellar dipole magnetic field. The hydrodynamic equations are solved to determine the velocity, density and temperature profiles of the flow. We use accreting magnetic white-dwarf stars as an illustrative example of astrophysical applications. Our calculations show that the compressional heating due to the field geometry is as important as radiative cooling and gravity in determining the structure of the post-shock flow in accreting white-dwarf stars. The generalisation of the formulation to accretion flows channelled by higher-order fields and the applications to other astrophysical systems are discussed.

We present the results of XMM-Newtonobservations of four AM CVn systems – AM CVn, CR Boo, HP Lib and GP Com. Their light curves show very different characteristics. The X-ray light curves show no coherent pulsations, suggesting the accreting white dwarfs have relatively low magnetic field strengths. Their spectra were best modelled using a multi-temperature emission model and a strong UV component. We find that CR Boo and HP Lib have X-ray spectra with abundances consistent with relatively low temperature CNO processed material, while AM CVn and GP Com show an enhancement of nitrogen. A large fraction of the accretion luminosity is emitted in the UV. We determine accretion luminosities of ~$1.6\times10^{33}$erg s-1and $1.7\times10^{31}$erg s-1for AM CVn and GP Com respectively. Comparing the implied mass transfer rates with that derived using model fits to optical and UV spectra, we find evidence that in the case of AM CVn, we do not detect a significant proportion of the accretion energy. This missing component could be lost in the form of a wind.

We present high time-resolution optical energy-resolved photometry of the eclipsing cataclysmic variable V2301 Oph made using the ESA S-Cam detector, an array of photon counting super-conducting tunnel junction (STJ) devices with intrinsic energy resolution. Three eclipses were observed, revealing considerable variation in the eclipse shape, particularly during ingress. The eclipse shape is shown to be understood in terms of AM Her accretion via a bright stream, with very little contribution from the white dwarf photosphere and/or hotspot. About two thirds of the eclipsed light arises in the threading region. Variation in the extent of the threading region can account for most of the variations observed between cycles. Spectral fits to the data reveal a 10 000 K blackbody continuum with strong, time-varying emission lines of hydrogen and helium. This is the first time that stellar emission lines have been detected in the optical band using a non-dispersive photon-counting system.

We have used ISO to observe the Magnetic Cataclysmic Variable AE Aquarii in the previously unexplored range from 4.8 μm up to 170 μm in the framework of a coordinated multi-wavelength campaign from the radio to optical wavelengths. We have obtained for the first time a spectrum between 4.8 and 7.3 μm with ISOCAM and ISOPHOT-P: the major contribution comes from the secondary star spectrum, with some thermal emission from the accretion stream, and possibly some additional cyclotron radiation from the post-shock accretion material close to the magnetised white dwarf. Having reprocessed ISOPHOT-C data, we confirm AE Aqr detection at $90~\mu$m and we have re-estimated its upper limit at 170 μm. In addition, having re-processed IRAS data, we have detected AE Aqr at 60 μm and we have estimated its upper limits at 12, 25, and 100 μm. The literature shows that the time-averaged spectrum of AE Aqr increases roughly with frequency from the radio wavelengths up to ${\sim} 761~ \mu$m; our results indicate that it seems to be approximately flat between ~761 and ${\sim} 90 ~\mu$m, at the same level as the 3σupper limit at 170 μm; and it then decreases from ${\sim} 90~ \mu$m to ${\sim} 7~ \mu$m. Thermal emission from dust grains or from a circum-binary disc seems to be very unlikely in AE Aqr, unless such a disc has properties substantially different from those predicted recently. Since various measurements and the usual assumptions on the source size suggest a brightness temperature below 109K at $\lambda \leq 3.4$mm, we have reconsidered also the possible mechanisms explaining the emission already known from the submillimetre to the radio. The complex average spectrum measured from ${\sim} 7 ~\mu$m to the radio must be explained by emission from a plasma composed of more than one “pure” non-thermal electron energy distribution (usually assumed to be a power-law): either a very large volume (diameter ≥80 times the binary separation) could be the source of thermal bremsstrahlung which would dominate from ${\sim} 10 ~\mu$m to the ~millimetre, with, inside, a non-thermal source of synchrotron which dominates in radio; or, more probably, an initially small infrared source composed of several distributions (possibly both thermal, and non-thermal, mildly relativistic electrons) radiates gyro-synchrotron and expands moderately: it requires to be re-energised in order to lead to the observed, larger, radio source of highly relativistic electrons (in the form of several non-thermal distributions) which produce synchrotron.

We present the first X-ray observation of Jupiter by XMM-Newton. Images taken with the EPIC cameras show prominent emission, essentially all confined to the 0.2-2.0 keV band, from the planet's auroral spots; their spectra can be modelled with a combination of unresolved emission lines of highly ionised oxygen (OVII and OVIII), and a pseudo-continuum which may also be due to the superposition of many weak lines. A 2.8σenhancement in the RGS spectrum at 21-22 Å (~0.57 keV) is consistent with an OVII identification. Our spectral analysis supports the hypothesis that Jupiter's auroral emissions originate from the capture and acceleration of solar wind ions in the planet's magnetosphere, followed by X-ray production by charge exchange. The X-ray flux of the North spot is modulated at Jupiter's rotation period. We do not detect evidence for the ~45 min X-ray oscillations observed by Chandramore than two years earlier. Emission from the equatorial regions of the planet's disk is also observed. Its spectrum is consistent with that of scattered solar X-rays.

We present results from the XMM-Newtonobservations of the dwarf nova YZ Cnc in a quiescent state. We have performed a detailed time series analysis of the resulting light curves. Unusually, we do not detect any orbital modulation in the UV, with only marginal evidence for X-ray modulation on this period. Although there are peaks in the X-ray periodograms at periods less than 5000 s, we attribute them to red noise effects and assign significance to them using a novel approach. The variability in the UV and optical bands can also be modelled as a result of aperiodic variability (red noise) in the system. There is evidence that the UV and X-ray fluxes are anti-correlated with a time delay of about 100 s, with the UV lagging behind the X-ray emission. This anti-correlation is intriguing, but is only present on two occasions lasting several 1000 s each. The X-ray spectrum shows similar emission features to other dwarf novae and is well fitted using a multi-temperature emission model. We measure a relatively high X-ray luminosity of ${\sim}1.4\times 10^{32}$ergs/s, although this is consistent with a low binary inclination. Finally, we find evidence for a possible -1200 km s-1blue shift in the fitted Fe K line energies, possibly indicating the presence of an outflow in this low inclination system.

We revisit the XMM-Newtonobservations of the dwarf nova OY Car taken in July 2000 which occured shortly after an outburst. Ramsay et al. ([CITE]) found a prominent energy dependent modulation at a period of 2240 s: this modulation was only seen for ~1/3 of the observation duration. In our new analysis, we examine this time interval in greater detail. In addition to the 2240 s period we find evidence for other periods, the most prominent being near 3500 s. Both these modulations are most likely due to changes in photoelectric absorption over this period: this is supported by phase-resolved spectroscopy. This may indicate the presence of matter above the accretion disc or a presence of a magnetic accretion curtain. In this case the 2240 s period could represent a spin period of the white dwarf and the 3500 s period a beat period between the spin and orbital periods. We also model the Bband and UV eclipse profiles and light curves using a new technique to map the spatial extent of the accretion disc. As a result we find that whilst the optical emission is dominated by both the emission close to the accretion disc boundary layer and the hot spot where the accretion stream hits the disc, the UV emission is mainly dominated by the inner disc/boundary layer only.

We present the high resolution spectrum of the isolated neutron star RX J0720.4-3125, obtained with the Reflection Grating Spectrometer on XMM-Newton, complemented with the broad band spectrum observed with the EPIC PN camera. The spectrum appears smooth, with no evidence for strong photospheric absorption or emission features. We briefly discuss the implications of our failure to detect structure in the spectrum.

We model the spin pulse intensity and hardness ratio profiles of the isolated neutron star RX J0720.4-3125 using XMM-Newtondata. The observed variation is approximately sinusoidal with a peak-to-peak amplitude of 15% , and the hardness ratio is softest slightly before flux maximum. By using polar cap models we are able to derive maximum polar cap sizes and acceptable viewing geometries. The inferred sizes of the caps turn out to be more compatible with a scenario in which the neutron star is heated by accretion, and place limits on the magnetic field strength. The hardness ratio modulation can then be explained in terms of energy-dependent beaming effects, and this constrains the acceptable models of the emerging radiation to cases in which softer photons are more strongly beamed than harder photons. An alternative explanation in terms of spatially variable absorption co-rotating in the magnetosphere is also discussed.

We present XMM-Newtonobservations of the eclipsing, disc accreting, cataclysmic variable OY Car which were obtained as part of the performance verification phase of the mission. The star was observed 4 days after an outburst and then again 5 weeks later when it was in a quiescent state. There is a quasi-stable modulation of the X-rays at ~2240 s, which is most prominent at the lowest energies. We speculate that this may be related to the spin period of the white dwarf. The duration of the eclipse ingress and egress in X-rays is 20-30 s. This indicates that the bulk of the X-ray emission originates from the boundary layer which has a negligible height above the surface of the white dwarf. The eclipse profile implies a white dwarf of mass $M_{1}=0.9{-}1.1$$M_{\odot}$and a secondary star of $M_{2}=0.08{-}0.11$$M_{\odot}$.

We present XMM-NewtonX-ray spectra of the disc accreting cataclysmic variable OY Car, which were obtained during the performance verification phase of the mission. These data were taken 4 days after a short outburst. In the EPIC spectra we find strong iron Kαemission with weaker iron Kβemission together with silicon and sulphur lines. The spectra are best fitted with a three temperature plasma model with a partial covering absorber. Multiple temperature emission is confirmed by the emission lines seen in the RGS spectrum and the H/He like intensity ratio for iron and sulphur which imply temperatures of ~7 keV and ~3 keV respectively.

IntroductionGiven the importance placed on awareness and participation in research by Speciality and Training organisations, we sought to survey Scottish trainee attitudes to exposure to research practice during training and research in or out of programme.MethodsAn online survey was distributed to core and specialist trainees in general surgery in Scotland.ResultsOver a 4-month period, 108 trainees (75 ST/SPRs and 33 CTs) completed the survey. In their current post, most were aware of ongoing research projects (77%) and 55% were aware of trial recruitment. Only 47% attend regular journal clubs. Most believe that they are expected to present (89%) and publish (82%) during training. Most (59%) thought that participation in research is well supported. 57% were advised to undertake time out of programme research, mostly by consultants (48%) and training committee (36%). Of the 57 with time out of programme research experience, most did so in early training (37%) or between ST3-5 (47%). 28 out of the 36 (78%) without a national training number secured one after starting research. Most undertook research in a local academic unit (80%) funded by small grants (47%) or internally (33%). Most research (69%) was clinically orientated (13/55 clinical, 25/55 translational). 56% of those completing time out of programme research obtained an MD or PhD. About 91% thought that research was relevant to a surgical career.ConclusionsMost trainees believe that research is an important part of training. Generally, most trainees are exposed to research practices including trial recruitment. However, <50% attend regular journal clubs, a pertinent point, given the current ‘exit exam’ includes the assessment of critical appraisal skills.

Abstract: The pea (Pisum sativum L.) varieties Baroness (United Kingdome) and Baccara (France) were transformed via Agrobacterium tumefaciens-mediated gene transfer with pGPTV binary vectors containing the bar gene in combination with two different antifungal genes coding for polygalacturonase-inhibiting protein (PGIP) from raspberry (Rubus idaeus L.) driven by a double 35S promoter, or the stilbene synthase (Vst1) from grape (Vitis vinifera L.) driven by its own elicitor-inducible promoter. Transgenic lines were established and transgenes combined via conventional crossing. Resveratrol, produced by Vst1 transgenic plants, was detected using HPLC and the PGIP expression was determined in functional inhibition assays against fungal polygalacturonases. Stable inheritance of the antifungal genes in the transgenic plants was demonstrated.

A reproducible and efficient transformation method was developed for Desi and Kabuli chickpeas ( Cicer arietinum L.) using germinated seedlings as sources of explants. Slices derived from plumules were the most efficient at generating transformed shoots. The AGL1 Agrobacterium-treated explants were first incubated on thidiazuron-containing media, then selected using phosphinothricin. Resistant shoots were successfully transferred to soil either by grafting or in vitro rooting. In experiments each taking 4–9 months, a total of 41 confirmed transformed lines were created using embryo axis slices as source explants, giving a transformation frequency of 5.1%. Southern analysis and histochemical and leaf painting assays demonstrated integration and expression of the transgenes in the initial transformants and two generations of progeny.

Accretion in white–dwarf binary systems can occur through discs, accretion columns or a combination of these, depending on the magnetic field of the white dwarf. Recent high–quality X–ray observations with the XMM–Newton and Chandra observatories have significantly advanced our understanding of the physics of the accretion process, and place severe tests on our existing models. There have been some surprises, such as the strong dependence of atmospheric heating on accretion rate. However, we believe that we are now confident that we understand in general the physical processes in the accretion region, although some complicating factors, such as absorption, remain. We also discuss new developments in ultra–short–period white–dwarf binary systems.

This study investigated the relationship of the hepatosplanchnic production and uptake of inflammatory mediators, hepatosplanchnic perfusion, and outcome during major abdominal surgery to evaluate the hypothesis that regional production of inflammatory mediators precedes the development of hepatic dysfunction. This retrospective analysis of data and blood samples collected during a randomized controlled clinical trial included high-risk surgical patients undergoing major abdominal surgery in a 24-bed university-afilliated intensive care unit. Patients were divided into a subgroup that developed hepatic dysfunction (HD) postoperatively and a subgroup without hepatic dysfunction (HD−). Hepatic vein and arterial plasma levels of IL-6, IL-8, s-E-selectin, s-ICAM-1, and the TNF-receptors 55 and 75 were measured, and the flux was calculated by multiplying the difference in hepatic vein minus arterial levels of the mediators by the hepatosplanchnic flow. Systemic (thermodilution) and total hepatosplanchnic blood flow (using indocyanine green ICG-dilution method) and gastric intramucosal pH (pHi) were assessed preoperatively, 4, 24, and 36 h postoperatively. Of a total of 26 patients, 6 patients developed hepatic dysfunction after their abdominal surgery (mean 6 days postoperatively). The number of sepsis-related deaths and postoperative days on the ventilator were significantly higher in this group. A higher production of IL-8, TNF-receptor-75 and 55 in the hepatosplanchnic area in the HD subgroups was found, which preceded the development of organ dysfunction (P0.04, P0.02, and P0.02, respectively). Moreover, the uptake of s-ICAM-1 was significantly increased in this subgroup. Furthermore, total hepatosplanchnic blood flow was significantly higher and pHi was significantly lower in the HD group, whereas global hemodynamic data were similar in the two subgroups. In conclusion, the development of postoperative organ dysfunction is preceded by an increased regional inflammatory response, indicated by an increased soluble TNF-receptor shedding and IL-8 production from the hepatosplanchnic area together with an increased uptake of s-ICAM-1. Moreover, an increased total hepatosplanchnic blood flow with intramucosal acidosis was associated with this regional inflammatory response.

Abstract: PCR-based markers were developed from mononucleotide simple-sequence repeats in the chloroplast genome of Nicotiana tabacum and applied to the analysis of genetic diversity. These markers were found to detect high levels of polymorphism at three taxonomic levels in Solanaceous plants. Of 36 chloroplast loci examined, 26 show some degree of polymorphism among potato accessions. Among a set of 30 tetraploid potato cultivars it is apparent that a single chloroplast haplotype is prevalent, presumably a result of the widespread use as a female parent of the imported US cultivar Rough Purple Chili in the latter half of the 19th century. Nonetheless, there is considerable chloroplast diversity in the cultivated potato, and it is clear that a large proportion of this variability has arisen through the use of wild or primitive cultivated species of potato in introgression programmes. This variability should be used in future breeding programmes. An examination of single accessions from 24 potato species, as well as representatives from tobacco and other members of the Solanaceae, reveals high levels of inter-specific chloroplast DNA variation. These data, and the ease of use and potential for multiplexing of these markers, suggest that cpSSRs will be of great utility in population genetics, germplasm management, evolutionary and phylogenetic studies as well as in, the analysis of material from introgression and somatic-fusion experiments. Interestingly, the polymorphism arising from one of the more-polymorphic chloroplast loci examined, does not originate solely from the SSR, and is due to variation in the copy number of two tandemly arrayed sequence elements.

The putative transforming proteins of the four acute leukaemia viruses belonging to the MC29 subgroup were shown to be phosphorylated in vivo. Comparison of the MC29 and CM11 encoded phosphoproteins revealed identical tryptic phosphopeptide maps, with both the gag and myc domains being phosphorylated. In contrast, the MH2 phosphoprotein was only phosphorylated on the gag domain. Analysis of partial transformation‐defective MC29 deletion mutants revealed that the deletions had removed the v‐myc specific phosphopeptides. Phosphoamino acid analysis showed that these deleted phosphopeptides were phosphorylated on threonine. Moreover, a back mutant that had regained transforming ability had regained these phosphopeptides. These studies correlate the phosphorylation of the gag‐myc protein with the transformation capability of the virus.

Passive immunization with antibody to the core region of endotoxin (core lipopolysaccharide (LPS)) has been reported to reduce mortality in severe sepsis. A rat model of endotoxaemia that reproduces the hyperdynamic cardiovascular state seen in early sepsis was developed to test monoclonal antibodies specific for core LPS. A thermodilution technique of measuring cardiac output was adapted for use in rats. Twenty-five animals were anaesthetized and mechanically ventilated with monitoring of central venous pressure and mean arterial pressure. Fluid replacement was adjusted to maintain the central venous pressure. Controls (n= 10) and antibody-treated animals (n= 5) showed no significant change in cardiac output. Animals given 0.1 mg kg−1R2 endotoxin over 1 h (n= 5) showed a significant rise in cardiac output of 65 per cent (P< 0.01). This was abolished in rats given both antibody and endotoxin (n= 5). This study provides evidence that a monoclonal antibody against core LPS abolishes the hyperdynamic state induced by endotoxin infusion.

We postulate in this paper that highly structured speech production models will have much to contribute to the ultimate success of speech recognition in view of the weaknesses of the theoretical foundation underpinning current technology. These weaknesses are analyzed in terms of phonological modeling and of phonetic-interface modeling. We present two probabilistic speech recognition models with the structure designed based on approximations to human speech production mechanisms, and conclude by suggesting that many of the advantages to be gained from interaction between speech production and speech recognition communities will develop from integrating production models with the probabilistic analysis-by-synthesis strategy currently used by the technology community.

Acquired infection is a common problem in intensive care and in a general ICU the infection rate can exceed 80% in patients ventilated beyond 5 days. SDD, adapted from regimes used in neutropenic patients, was first introduced to the ICU situation in Groningen. This article reviews 10 published trials of SDD in ICU. The trial designs vary but all show a significant reduction in both colonisation rates and acquired infection rates. Infection rates were reduced from 10%–78% to 3%–10% in the SDD treated groups. Of the 10 trials 2 showed an overall reduction in mortality 2 showed a reduction in infection-related mortality and 1 showed a reduction in mortality amongst trauma patients. Although further evaluation of trials is required SDD now appears to be of proven efficacy in certain groups of high risk patients within ICU.

N-myc is a gene whose amplification has been implicated in the genesis of several malignant human tumors. We have identified two proteins with molecular weights of 65,000 and 67,000 encoded by N-myc. The abundance of these proteins in tumor cells was consonant with the extent of amplification of N-myc. The two proteins apparently arose from the same mRNA, were phosphorylated, were exceptionally unstable, were located in the nucleus of cells, and bound to both single- and double-stranded DNA. These properties suggest that the products of N-myc and of the related proto-oncogene c-myc may have similar biochemical functions and that N-myc may be a regulatory gene. Our findings sustain the view that inordinate expression of N-myc may contribute to the genesis of several different human tumors.

The mogoplistine cricket Ornebius apertaOtte & Alexander 1983 is established in the Auckland region. It may be recognised by its characteristic song but as it is ventriloquistic and retiring only 1 specimen has as yet been collected. A similar if not identical species was collected at Paihia, Northland, in 1977. The Auckland population is either an extension of the range of this species or newly-immigrated.

Since its first description in 1967, the mortality of the adult respiratory distress syndrome (ARDS) has remained unchanged despite the increasing sophistication of supportive techniques. Few patients now die of refractory hypoxemia, the majority succumbing to the multiple systems organ failure syndrome, commonly due to sepsis. Sepsis is both the most common cause of ARDS, usually involving the abdomen, and the most frequent complication, usually affecting the lungs. ARDS is, thus, increasingly seen as the pulmonary component of multiple systems organ failure, triggered by the systemic response to sepsis.

Damage to the protooncogene MYC has been implicated in the genesis of diverse human tumors, but the tumorigenic potential of the isolated gene has been disputed. Here we report the use of a retroviral vector to test the potency of human MYC for neoplastic transformation in avian cells. We found that sustained and abundant expression of MYC can transform both embryonic fibroblasts and hematopoietic cells and elicit granulocytic leukemias in chickens. Transformation by MYC is accompanied by changes in diverse aspects of cellular phenotype, including morphology, ability to grow in suspension, rate of proliferation, the structure of the cytoskeleton, and the composition of the extracellular matrix. Nevertheless, the biological potency of MYC is inherently constrained when compared to that of the retroviral oncogene v-myc. Our findings enlarge on previous descriptions of neoplastic transformation by MYC and sustain the view that ungoverned expression of the gene can contribute to the genesis of human tumors.

The myb proto-oncogenes are thought to have a role in the cell division cycle. We have examined this possibility by genetic analysis in Drosophila melanogaster, which possesses a single myb gene. We have described previously two temperature-sensitive, recessive lethal mutants in Drosophila myb (Dm myb). The phenotypes of these mutants revealed a requirement for myb in diverse cellular lineages throughout the course of Drosophila development. We now report a cellular explanation for these findings by showing that Dm myb is required for both mitosis and prevention of endoreduplication in wing cells. Myb apparently acts at or near the time of the G2/M transition. The two mutant alleles of Dm myb produce the same cellular phenotype, although the responsible mutations are located in different functional domains of the gene product. The mutant phenotype can be partially suppressed by ectopic expression of either cdc2 or string, two genes that are known to promote the transition from G2 to M. We conclude that Dm myb is required for completion of cell division and may serve two independent functions: promotion of mitosis, on the one hand, and prevention of endoreduplication when cells are arrested in G2, on the other.

Initial resistance of bacterial infection is mediated primarily by polymorphonuclear leucocytes (PMN). Anaesthetic agents have been reported to impair various aspects of PMN function. It is possible that the use of these agents to sedate critically ill patients may further compromise an already depressed host defence mechanism. A flow cytometric technique with fresh whole blood from 10 healthy volunteers was used. Phagocytic and respiratory burst activity of PMN incubated for 1 h with either propofol, thiopentone, midazolam or ketamine at both clinical plasma concentrations and 100 times this concentration were determined. Thiopentone at the higher concentration reduced both respiratory burst activity (mean peak channel 50.7 compared with control value of 77.6 (P < 0.0001)) and phagocytosis (mean peak channel 47.5 compared with 79.9 (P < 0.0001)). Ketamine at 100 times the clinical plasma concentration also reduced respiratory burst and phagocytosis, but this failed to reach statistical significance (P = 0.10 and P = 0.053, respectively). No significant depression occurred in the other groups. The results suggest that these i.v. anaesthetic agents, at clinically relevant concentrations, have minimal effects on PMN phagocytosis and oxygen free radical production. At higher concentrations thiopentone and ketamine may affect phagocytic function and thiopentone may impair intracellular cytolysis.

The proto-oncogene c-myc may play a role in controlling the growth and division of normal cells, and abnormalities of the gene have been implicated in the genesis of a substantial variety of human tumors. To facilitate further study of these issues, we developed antisera that permit the identification and isolation of the protein encoded by the human and other mammalian versions of c-myc. We found that c-myc(human) gives rise to at least two phosphoproteins with apparent molecular weights of 62,000 [pp62c-myc(human), the major product] and 66,000 [pp66c-myc(human), produced in smaller quantities and possibly a modified version of the Mr 62,000 protein]. Both proteins have relatively short half-lives of approximately equal to 30 min. Mouse c-myc encodes similar proteins with molecular weights of 64,000 and 66,000. The use of cells transformed by DNA-mediated gene transfer sustained previous deductions that the entire coding domain of c-myc(human) is contained in the second and third exons of the gene and resolved previous ambiguities by showing that analogous exons specify the entire protein product of c-myc(chicken). Tumor cells containing amplification of c-myc(human) produce relatively large amounts of pp62/pp66c-myc(human). By contrast, translocations of c-myc found in cells derived from Burkitt lymphoma appear merely to sustain expression of c-myc(human) at levels found also in nontumorigenic lymphoblastoid cells, rather than to increase expression of the gene to manifestly abnormal levels.