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Se cuantificaron las principales fuentes emisoras de CO2e en la Universidad Técnica Nacional sede Atenas (UTNSA) y se relacionó con el promedio por estudiantes desde el 2012 y hasta 2015 como línea base para planificar el balance de carbono en busca de la neutralidad. Se utilizó la metodología del Grupo Intergubernamental de Expertos en Cambio Climático (IPCC) planteada en el 2006 y los factores de emisión publicados por el Instituto Meteorológico Nacional (IMN) 2016. Se identificaron ocho fuentes de emisiones, seis directas y dos indirectas, siendo estas: semovientes, residuos ordinarios, combustibles, aguas residuales, fertilizantes nitrogenados, electricidad, gas licuado de petróleo (GLP) y extintores de CO2, según su orden de importancia. Las tres primeras fuentes emitieron el 93% del total de emisiones de la UTN-SA. Al desglosar las emisiones se determinan tres patrones: las que aumentan las emisiones, las que se mantienen y las que disminuyen a pesar del incremento de estudiantes. En general las emisiones totales incrementan al aumentar el número de estudiantes, pero al mismo tiempo las emisiones por estudiante disminuyen.

We present optical light curves, redshifts, and classifications for 365 spectroscopically confirmed Type Ia supernovae (SNe Ia) discovered by the Pan-STARRS1 (PS1) Medium Deep Survey. We detail improvements to the PS1 SN photometry, astrometry and calibration that reduce the systematic uncertainties in the PS1 SN Ia distances. We combine the subset of 279 PS1 SN Ia ($0.03 < z < 0.68$) with useful distance estimates of SN Ia from SDSS, SNLS, various low-z and HST samples to form the largest combined sample of SN Ia consisting of a total of 1048 SN Ia ranging from $0.01 < z < 2.3$, which we call the `Pantheon Sample'. When combining Planck 2015 CMB measurements with the Pantheon SN sample, we find $��_m=0.307\pm0.012$ and $w = -1.026\pm0.041$ for the wCDM model. When the SN and CMB constraints are combined with constraints from BAO and local H0 measurements, the analysis yields the most precise measurement of dark energy to date: $w0 = -1.007\pm 0.089$ and $wa = -0.222 \pm0.407$ for the w0waCDM model. Tension with a cosmological constant previously seen in an analysis of PS1 and low-z SNe has diminished after an increase of $2\times$ in the statistics of the PS1 sample, improved calibration and photometry, and stricter light-curve quality cuts. We find the systematic uncertainties in our measurements of dark energy are almost as large as the statistical uncertainties, primarily due to limitations of modeling the low-redshift sample. This must be addressed for future progress in using SN Ia to measure dark energy., Accepted by ApJ. Data can be found here: http://dx.DOI.org/10.17909/T95Q4X

We present photometric and spectroscopic observations of a luminous Type IIP Supernova (SN) 2009kf discovered by the Pan-STARRS 1 (PS1) survey and also detected by the Galaxy Evolution Explorer. The SN shows a plateau in its optical and bolometric light curves, lasting approximately 70 days in the rest frame, with an absolute magnitude of M_V = -18.4 mag. The P-Cygni profiles of hydrogen indicate expansion velocities of 9000 km s^(-1) at 61 days after discovery which is extremely high for a Type IIP SN. SN 2009kf is also remarkably bright in the near-ultraviolet (NUV) and shows a slow evolution 10-20 days after optical discovery. The NUV and optical luminosity at these epochs can be modeled with a blackbody with a hot effective temperature (T ~ 16,000 K) and a large radius (R ~ 1 × 10^(15) cm). The bright bolometric and NUV luminosity, the light curve peak and plateau duration, the high velocities, and temperatures suggest that 2009kf is a Type IIP SN powered by a larger than normal explosion energy. Recently discovered high-z SNe (0.7 < z < 2.3) have been assumed to be IIn SNe, with the bright UV luminosities due to the interaction of SN ejecta with a dense circumstellar medium. UV-bright SNe similar to SN 2009kf could also account for these high-z events, and its absolute magnitude M_(NUV) = -21.5 ± 0.5 mag suggests such SNe could be discovered out to z ~ 2.5 in the PS1 survey.

Supernova (SN) Refsdal is the first multiply-imaged, highly-magnified, and spatially-resolved SN ever observed. The SN exploded in a highly-magnified spiral galaxy at z=1.49 behind the Frontier Fields Cluster MACS1149, and provides a unique opportunity to study the environment of SNe at high z. We exploit the time delay between multiple images to determine the properties of the SN and its environment, before, during, and after the SN exploded. We use the integral-field spectrograph MUSE on the VLT to simultaneously target all observed and model-predicted positions of SN Refsdal. We find MgII emission at all positions of SN Refsdal, accompanied by weak FeII* emission at two positions. The measured ratios of [OII] to MgII emission of 10-20 indicate a high degree of ionization with low metallicity. Because the same high degree of ionization is found in all images, and our spatial resolution is too coarse to resolve the region of influence of SN Refsdal, we conclude that this high degree of ionization has been produced by previous SNe or a young and hot stellar population. We find no variability of the [OII] line over a period of 57 days. This suggests that there is no variation in the [OII] luminosity of the SN over this period, or that the SN has a small contribution to the integrated [OII] emission over the scale resolved by our observations., Comment: 5 pages, 4 figures, accepted for publication in A&A

We present a high-precision mass model of galaxy cluster Abell 2744, based on a strong-gravitational-lensing analysis of the \emph{Hubble Space Telescope Frontier Fields} (HFF) imaging data, which now include both \emph{Advanced Camera for Surveys} and \emph{Wide-Field Camera 3} observations to the final depth. Taking advantage of the unprecedented depth of the visible and near-infrared data, we identify 34 new multiply imaged galaxies, bringing the total to 61, comprising 181 individual lensed images. In the process, we correct previous erroneous identifications and positions of multiple systems in the northern part of the cluster core. With the \textsc{Lenstool} software and the new sets of multiple images, we model the cluster using two cluster-scale dark matter halos plus galaxy-scale halos for the cluster members. Our best-fit model predicts image positions with an \emph{RMS} error of 0.69$\arcsec$, which constitutes an improvement by almost a factor of two over previous parametric models of this cluster. We measure the total projected mass inside a 200~kpc aperture as ($2.162\pm 0.005$)$\times 10^{14}M_{\odot}$, thus reaching 1\% level precision for the second time, following the recent HFF measurement of MACSJ0416.1-2403. Importantly, the higher quality of the mass model translates into an overall improvement by a factor of 4 of the derived magnification factor. % for the high-redshift lensed background galaxies. Together with our previous HFF gravitational lensing analysis, this work demonstrates that the HFF data enables high-precision mass measurements for massive galaxy clusters and the derivation of robust magnification maps to probe the early Universe., 11 pages, 4 figures, 3 tables, Accepted for publication in MNRAS. arXiv admin note: text overlap with arXiv:1405.3582

Maryland's recently created oyster restored reefs provide us with a unique opportunity to observe the abundance and species composition of macrofauna assemblages on unexploited reefs with high concentrations of mature oysters and undisturbed reef architecture. They might thus be used to better understand the magnitude of losses to reef dwelling macrofauna communities, and the associated loss of ecological functions resulting from reef destruction. We sampled reef macrofaunal assemblages on restored plots at four restored oyster reefs and adjacent non-restored plots located outside restored boundaries. We then compared the effects of study site location, and habitat quality (restored versus non-restored) on macrofaunal density using thirteen response variables. Density of macrofauna was an order of magnitude higher on restored reefs, epifaunal density was more than twice as high on restored reefs and sessile macrofaunal density was two orders of magnitude higher on restored reefs. Three out of the five dominant taxonomic groups were much more abundant on restored plots. Mean amphipod density was 20 times higher on restored plots and densities of xanthid crabs and demersal fish were both four times greater on restored plots. Two out of four functional feeding groups: suspension feeders and carnivore/omnivores, were more abundant on restored plots. Since reef macrofauna include many important fish prey species, oyster reef restoration may have the potential to augment fish production by increasing fish prey densities and fish foraging efficiency.

We present griz light curves of 146 spectroscopically confirmed Type Ia Supernovae ($0.03 < z, Comment: 38 pages, 16 figures, 14 tables, ApJ in press

To evaluate the potential of unleaded gasoline vapor for developmental toxicity, a sample was prepared by slowly heating API 94 ‐ 02 (1990 industry average gasoline) and condensing the vapor. The composition of this vapor condensate, which comprises 10.4% by volume of the starting gasoline, is representative of real-world exposure to gasoline vapor encountered at service stations and other occupational settings and consists primarily of volatile short chain (C4-C6) aliphatic hydrocarbons (i.e. paraffins) with small amounts of cycloparaffins and aromatic hydrocarbons. A preliminary study in rats and mice resulted in no developmental toxicity in either species. However, a slight reduction in maternal body weight gain in rats led to the selection of rats for this guideline study. Groups of pregnant rats ( n 5 24/group) were exposed to unleaded gasoline vapor at concentrations of 0, 1000, 3000, or 9000 (75% lower explosive limit) ppm equivalent to 0, 2653, 7960, or 23900 mg/m 3 , for 6 h/day on gestation days 6 ‐19. All rats were sacrificed on gestation day 20. No maternal toxicity was observed. Developmentally, there were no differences between treated and control groups in malformations, total variations, resorptions, fetal body weight, or viability. The maternal and developmental NOAEL is 9000 ppm. Under conditions of this study, unleaded gasoline vapors did not produce evidence of developmental toxicity. © 2001 Elsevier Science Inc. All rights reserved.

We present optical photometric and spectroscopic coverage of the superluminous supernova (SLSN) PS1-11ap, discovered with the Pan-STARRS1 Medium Deep Survey at z = 0.524. This intrinsically blue transient rose slowly to reach a peak magnitude of M_u = -21.4 mag and bolometric luminosity of 8 x 10^43 ergs^-1 before settling onto a relatively shallow gradient of decline. The observed decline is significantly slower than those of the superluminous type Ic SNe which have been the focus of much recent attention. Spectroscopic similarities with the lower redshift SN2007bi and a decline rate similar to 56Co decay timescale initially indicated that this transient could be a candidate for a pair instability supernova (PISN) explosion. Overall the transient appears quite similar to SN2007bi and the lower redshift object PTF12dam. The extensive data set, from 30 days before peak to 230 days after, allows a detailed and quantitative comparison with published models of PISN explosions. We find that the PS1-11ap data do not match these model explosion parameters well, supporting the recent claim that these SNe are not pair instability explosions. We show that PS1-11ap has many features in common with the faster declining superluminous Ic supernovae and the lightcurve evolution can also be quantitatively explained by the magnetar spin down model. At a redshift of z = 0.524 the observer frame optical coverage provides comprehensive restframe UV data and allows us to compare it with the superluminous SNe recently found at high redshifts between z = 2-4. While these high-z explosions are still plausible PISN candidates, they match the photometric evolution of PS1-11ap and hence could be counterparts to this lower redshift transient., 19 pages, 10 figures, Accepted for publication in MNRAS

The Pan-STARRS1 (PS1) survey has obtained imaging in 5 bands (grizy_P1) over 10 Medium Deep Survey (MDS) fields covering a total of 70 square degrees. This paper describes the search for apparently hostless supernovae (SNe) within the first year of PS1 MDS data with an aim of discovering new superluminous supernovae (SLSNe). A total of 249 hostless transients were discovered down to a limiting magnitude of M_AB ~ 23.5, of which 76 were classified as Type Ia SNe. There were 57 SNe with complete light curves that are likely core-collapse SNe (CCSNe) or SLSNe and 12 of these have had spectra taken. Of these 12 hostless, non-Type Ia SNe, 7 were SLSNe of Type Ic at redshifts between 0.5-1.4. This illustrates that the discovery rate of Type Ic SLSNe can be maximised by concentrating on hostless transients and removing normal SNe Ia. We present data for two new possible SLSNe; PS1-10pm (z = 1.206) and PS1-10ahf (z = 1.1), and estimate the rate of SLSNe-Ic to be between 3^{+3}_{-2} * 10^{-5} and 8^{+2}_{-1} * 10^{-5} of the CCSNe rate within 0.3, 26 pages, 16 figures, Accepted for publication in MNRAS

Super-luminous supernovae that radiate more than 10^44 ergs per second at their peak luminosity have recently been discovered in faint galaxies at redshifts of 0.1-4. Some evolve slowly, resembling models of 'pair-instability' supernovae. Such models involve stars with original masses 140-260 times that of the Sun that now have carbon-oxygen cores of 65-30 solar masses. In these stars, the photons that prevent gravitational collapse are converted to electron-positron pairs, causing rapid contraction and thermonuclear explosions. Many solar masses of 56Ni are synthesized; this isotope decays to 56Fe via 56Co, powering bright light curves. Such massive progenitors are expected to have formed from metal-poor gas in the early Universe. Recently, supernova 2007bi in a galaxy at redshift 0.127 (about 12 billion years after the Big Bang) with a metallicity one-third that of the Sun was observed to look like a fading pair-instability supernova. Here we report observations of two slow-to-fade super-luminous supernovae that show relatively fast rise times and blue colours, which are incompatible with pair-instability models. Their late-time light-curve and spectral similarities to supernova 2007bi call the nature of that event into question. Our early spectra closely resemble typical fast-declining super-luminous supernovae, which are not powered by radioactivity. Modelling our observations with 10-16 solar masses of magnetar-energized ejecta demonstrates the possibility of a common explosion mechanism. The lack of unambiguous nearby pair-instability events suggests that their local rate of occurrence is less than 6x10^-6 times that of the core-collapse rate., Originally published in Nature, Oct 2013. Updated Oct 2016 to correct an error

We probe the systematic uncertainties from 113 Type Ia supernovae (SNIa) in the Pan-STARRS1 (PS1) sample along with 197 SN Ia from a combination of low-redshift surveys. The companion paper by Rest et al. (2013) describes the photometric measurements and cosmological inferences from the PS1 sample. The largest systematic uncertainty stems from the photometric calibration of the PS1 and low-z samples. We increase the sample of observed Calspec standards from 7 to 10 used to define the PS1 calibration system. The PS1 and SDSS-II calibration systems are compared and discrepancies up to ~0.02 mag are recovered. We find uncertainties in the proper way to treat intrinsic colors and reddening produce differences in the recovered value of w up to 3%. We estimate masses of host galaxies of PS1 supernovae and detect an insignificant difference in distance residuals of the full sample of 0.037\pm0.031 mag for host galaxies with high and low masses. Assuming flatness in our analysis of only SNe measurements, we find $w = {-1.120^{+0.360}_{-0.206}\textrm{(Stat)} ^{+0.269}_{-0.291}\textrm{(Sys)}}$. With additional constraints from BAO, CMB(Planck) and H0 measurements, we find $w = -1.166^{+0.072}_{-0.069}$ and $\Omega_M=0.280^{+0.013}_{-0.012}$ (statistical and systematic errors added in quadrature). Significance of the inconsistency with $w=-1$ depends on whether we use Planck or WMAP measurements of the CMB: $w_{\textrm{BAO+H0+SN+WMAP}}=-1.124^{+0.083}_{-0.065}$., Comment: 24 pages, 20 figures. Accepted by ApJ

Nature 502, 346–349 (2013); doi:10.1038/nature12569 In this Letter, we have identified an important error affecting Fig. 4 and Extended Data Fig. 6, as well as the values of some parameters derived from our model fits. We stress that this error in no way affects the discussion or the conclusions. Inbuilding the bolometric light curve of the superluminous supernova PTF 12dam, our code assumed that photometry from the Swift satellite was calibrated in the Vega magnitude system.

We precisely constrain the inner mass profile of Abell 2261 (z=0.225) for the first time and determine this cluster is not "over-concentrated" as found previously, implying a formation time in agreement with {\Lambda}CDM expectations. These results are based on strong lensing analyses of new 16-band HST imaging obtained as part of the Cluster Lensing and Supernova survey with Hubble (CLASH). Combining this with revised weak lensing analyses of Subaru wide field imaging with 5-band Subaru + KPNO photometry, we place tight new constraints on the halo virial mass M_vir = 2.2\pm0.2\times10^15 M\odot/h70 (within r \approx 3 Mpc/h70) and concentration c = 6.2 \pm 0.3 when assuming a spherical halo. This agrees broadly with average c(M,z) predictions from recent {\Lambda}CDM simulations which span 5

The Cluster Lensing And Supernova survey with Hubble (CLASH) is a 524-orbit multi-cycle treasury program to use the gravitational lensing properties of 25 galaxy clusters to accurately constrain their mass distributions. The survey, described in detail in this paper, will definitively establish the degree of concentration of dark matter in the cluster cores, a key prediction of CDM. The CLASH cluster sample is larger and less biased than current samples of space-based imaging studies of clusters to similar depth, as we have minimized lensing-based selection that favors systems with overly dense cores. Specifically, twenty CLASH clusters are solely X-ray selected. The X-ray selected clusters are massive (kT > 5 keV; 5 - 30 x 10^14 M_solar) and, in most cases, dynamically relaxed. Five additional clusters are included for their lensing strength (Einstein radii > 35 arcsec at z_source = 2) to further quantify the lensing bias on concentration, to yield high resolution dark matter maps, and to optimize the likelihood of finding highly magnified high-redshift (z > 7) galaxies. The high magnification, in some cases, provides angular resolutions unobtainable with any current UVOIR facility and can yield z > 7 candidates bright enough for spectroscopic follow-up. A total of 16 broadband filters, spanning the near-UV to near-IR, are employed for each 20-orbit campaign on each cluster. These data are used to measure precise (sigma_phz 1 to improve constraints on the time dependence of the dark energy equation of state and the evolution of such supernovae in an epoch when the universe is matter dominated.

Urea cycle disorders (UCDs) result from inherited defects in the ammonia detoxification pathway, leading to episodes of hyperammonaemia and encephalopathy. The purpose of this study was to answer the question, "what is the likely plasma amino acid profile of a patient known to have a UCD presenting with hyperammonaemia during acute metabolic decompensation", in order to support informed decisions regarding management.We analysed the results of plasma ammonia levels and amino acid profiles taken simultaneously or within 30 min of each other during acute admissions of all patients with a UCD at the Royal Children's Hospital, Melbourne, over 28 years. Samples from 96 admissions (79, 9 and 8 admissions for OTC, CPS and ASS deficiencies, respectively) from 14 patients fulfilled these criteria. Amino acid levels were measured by ion exchange chromatography with post-column ninhydrin derivatisation and interpreted in relation to age-related reference ranges.Plasma concentrations of all measured essential amino acids were low or low-normal in almost all samples. There was a strong positive correlation between low plasma branched-chain amino acids and other essential amino acids, and a negative correlation between ammonia and phenylalanine to tyrosine (Phe:Tyr) ratio in patients with OTC deficiency, and between glutamine and Phe:Tyr ratio in all patients, indicating protein deficiency.At admission, protein deficiency is common in patients with a UCD with hyperammonaemia. These results challenge the current guideline of stopping protein intake during acute decompensation in UCDs. Supplementation with essential amino acids (particularly branched-chain amino acids) at these times should be considered.

We present the discovery of two ultra-luminous supernovae (SNe) at z ~ 0.9 with the Pan-STARRS1 Medium-Deep Survey. These SNe, PS1-10ky and PS1-10awh, are amongst the most luminous SNe ever discovered, comparable to the unusual transients SN 2005ap and SCP 06F6. Like SN 2005ap and SCP 06F6, they show characteristic high luminosities (M_bol ~ -22.5 mag), blue spectra with a few broad absorption lines, and no evidence for H or He. We have constructed a full multi-color light curve sensitive to the peak of the spectral energy distribution in the rest-frame ultraviolet, and we have obtained time-series spectroscopy for these SNe. Given the similarities between the SNe, we combine their light curves to estimate a total radiated energy over the course of explosion of (0.9-1.4) x 10^51 erg. We find photospheric velocities of 12,000-19,000 km/s with no evidence for deceleration measured across ~3 rest-frame weeks around light-curve peak, consistent with the expansion of an optically-thick massive shell of material. We show that, consistent with findings for other ultra-luminous SNe in this class, radioactive decay is not sufficient to power PS1-10ky, and we discuss two plausible origins for these events: the initial spin-down of a newborn magnetar in a core-collapse SN, or SN shock breakout from the dense circumstellar wind surrounding a Wolf-Rayet star., Comment: Re-Submitted to ApJ

Objectives: To assess the needs of cancer patients for information about their condition and to understand the psychological impact of their illness. Background: The discussion of prognosis and treatment options in the palliative setting is an important and difficult part of oncology practice. To evaluate this, we examined the experiences of cancer patients of the physical and psychological impact of their disease on their life, and their opinions on the communication of end-of-life decisions and treatment options. Methods: A patient questionnaire was designed that encompassed communication regarding treatment and prognosis, quality-of-life attitudes subsequent to cancer diagnosis, end-of-life care and cancer drug funding. One hundred and twenty-five patients with a diagnosis of cancer were asked to participate and 96 questionnaires were completed and available for analysis. The questionnaire consisted of 63 questions and was completed in both an inpatient and outpatient setting. Results: This survey brought to light a number of controversial issues in cancer service provision, highlighting the emotional and psychological changes brought about by a cancer diagnosis. Major concerns of our patients include fear of death and pain, changes in interpersonal relationships and financial constraints. Only 66% of the patients wanted to be given a prognosis by their clinicians and just 70% of the patients recalled being given a detailed prognosis. 11% of the patients were not prepared to undergo palliative treatment. In all, 7% were not prepared to accept treatment for 1 year and 2% for 5 years of life in exchange for the potential side effects of cytotoxic chemotherapy. 12% of the patients would not want to be in possession of the information that they were in the terminal phase of the illness with a short time to live and 16% would not want this discussed with their next of kin. Conclusions: This study informs medical professionals about the importance of tailoring information to the needs of the individual patient, and we feel it provides insights into the successes and failures of our communication with cancer patients. It is important that difficult discussions are personalized to the individual patients’ wishes. These can vary dramatically both in the area of disclosure of bad news in prognosis and in end-of-life decision making. This study provides compelling evidence for good advanced care planning at an early stage in the management of patients with terminal cancers.

We examine the inner mass distribution of the relaxed galaxy cluster Abell 383 in deep 16-band HST/ACS+WFC3 imaging taken as part of the CLASH multi-cycle treasury program. Our program is designed to study the dark matter distribution in 25 massive clusters, and balances depth with a wide wavelength coverage to better identify lensed systems and generate precise photometric redshifts. This information together with the predictive strength of our strong-lensing analysis method identifies 13 new multiply-lensed images and candidates, so that a total of 27 multiple-images of 9 systems are used to tightly constrain the inner mass profile, $d\log \Sigma/d\log r\simeq -0.6\pm 0.1$ (r, Comment: 15 pages, 14 figures, 2 tabels; V3 matches the submitted version later published in ApJ

The 1- resonance at 512 keV in N-14 was measured precisely by detecting recoil protons after scattering C-13 beams on a thick CH2 target. Proton spectra were analyzed with a Breit-Wigner formalism. It is shown that energy loss and straggling of the protons and of the heavy ions in the target can be correctly taken into account.

A feasibility study was undertaken for the measurement of the resonance at E(r) = 545 keV in the N-13(p,gamma)O-14 reaction, using intense radioactive ion beams. The analog resonance at E(r) = 512 keV in C-12(p,gamma)N-14 was chosen as a test case, leading to improved knowledge of the resonance parameters. Thin- and thick-target yields were obtained with C-13 beams on an extended gas target and a polyethylene foil, respectively. In addition, thin and thick targets of enriched C-13 were irradiated with proton beams. Normalization problems arising with mixed ion beams (N-13/C-13) are discussed.

Alternating current dielectrophoresis in water was used to position graphite oxide soot (GO-soot) particles generated by rapid thermal expansion of graphite oxide under inert gas. The dielectrophoretic deposition was carried out at a frequency of 10 MHz and a peak-to-peak voltage of 10 V, and the deposited particles were analyzed using scanning electron microscopy. The vertical cross section, obtained by focused ion beam cutting, shows the wrinkled layers of the GO-soot particles and cavities between the layers. The electrical transport measurements show typical characteristics of metal-like pathways. The improved electrical contact between electrodes and GO-soot, probably due to the thin platelet structure of GO-soot, makes the material favorable for electrical device applications. The results demonstrate that AC dielectrophoresis can be used to selectively deposit graphite oxide soot particles at desired locations.

Introduction In 2011 patients referred with suspected colorectal cancer at our institution waited a median of 36 days (IQR28–46) for a treatment plan. This resulted in 61% of colorectal cancerstaking over 31 days to reach a decision to treat. We aimed to reduce the time spent in the diagnostic phase, which was perceived to be the main hold up in the fast track pathway. Methods A quality improvement approach was employed to change the new pathway from the existing clinic-first service to a straight-to-test service. The new nurse-led telephone triage service confirmed symptoms and assessed fitness for colonoscopy, with higher-risk patients defaulting to flexible sigmoidoscopy or clinic. Results for the first year of the new service are presented. Results 438 patients were referred between 1/10/2012 and 1/10/2013. 222 (50%) went straight to colonoscopy and 136 (31%) to flexible sigmoidoscopy, 46 (11%) went to clinic, 32(7%) patients did not attend and data was missing for 2(1%) patients. Final diagnoses are shown in the attached figure. Colorectal cancer was found in 14/358 patients (4%). Median time from receipt of referral to first endoscopy was 13 days (IQR 11–20), with 128/348 patients (29%) waiting more than 14 days. Median time to decision to treat colorectal cancer was 25 days (IQR 20–34) in straight to test patients, a significant reduction compared to 2010–2011 (p = 0.01), with 5/14 (36%) waiting more than 31 days. Median time to first oncological treatment was 40 days (IQR 28–44), with 1/14 (7%) waiting more than 62 days. 41/66 (62%) of patients with a normal colonoscopy were discharged directly from endoscopy back to their GP. Conclusion The new straight to test service was applicable to the majority of new colorectal fast track patients and a high patient uptake was observed. Colorectal cancer was in fact uncommon, which is being fed back to those referring into the system. Physical colorectal clinic appointments were saved in four-fifths of new patients and in two-thirds of those with a normal colonoscopy, which could be allocated to newly diagnosed cancers, or those requiring treatment for benign conditions. The straight to endoscopy service resulted in an average reduction of 11 days in making a treatment plan for new colorectal cancers. This contributed towards a low rate of breaches of the 62 day treatment target. However one-third of new cancer patients still waited over a month for a decision to treat, highlighting the extra time required for ancillary investigations and MDT discussion. These can be addressed by triggering staging investigations and MDT discussion at the time of endoscopy. Disclosure of Interest None Declared.

Maintaining good compliance is a major challenge in long-term cancer chemoprevention trials. Minimizing the number of inactive participants during a trial is an important factor in maximizing compliance. Identifying reasons for and predictors of inactivation is the first step in being able to reduce participant inactivation. In this skin cancer chemoprevention trial, the 2,297 participants were randomized to receive 25,000 IU of retinol daily or a placebo. Median follow-up time was 3.8 years. The reason for inactivation was determined for each participant who stopped taking the study capsules. Six hundred and seventy-seven (29.7%) participants became inactive during the 5-year study. There was no significant difference between the number of participants inactivating by treatment group or sex. The most common reasons for inactivation were illness of subject, spouse, or a close relative (18.6%) and experience of a clinical symptom consistent with vitamin A ingestion (17.1%). Participants in the vitamin A group (10.1%) more frequently cited symptoms coded as "not consistent with vitamin A" as the reason for inactivation compared with those in the placebo group [5.4% (P0.05)]. The inactivation rate was highest in the first month of the trial and declined thereafter. A low education level (hazard ratio, 1.59) and unmarried status (hazard ratio, 1.29) were the only significant predictors of inactivation. These findings may be useful in developing targeted strategies to decrease inactivation and thereby increase compliance in future chemoprevention trials. However, these findings need to be confirmed because published research in this area is very limited.

The objective of this study was to examine the effect of retinol and isotretinoin on the incidence of nonmelanoma skin cancer in high-risk subjects. A total of 525 participants with a history of at least four basal cell carcinomas (BCCs) and/or cutaneous squamous cell carcinomas (SCCs) were entered into a randomized, double-blind, placebo-controlled trial, performed in free-standing study clinics. Participants were randomly assigned to receive oral retinol (25,000 units), isotretinoin (5-10 mg), or placebo supplementation daily for 3 years. The time to first new occurrence of BCC or cutaneous SCC was used as the outcome measure. During the study period, 319 BCCs and 125 cutaneous SCCs were diagnosed clinically and pathologically. There were no differences between those who received retinol, isotretinoin, or the placebo, with regard to the time to first occurrence or to the total number of tumors noted. No beneficial effects were noted with regard to the prevention of nonmelanoma skin cancer with either retinol or isotretinoin.

We conducted a randomized, double-blind, controlled trial to examine the efficacy of retinol supplementation on the incidence of first new nonmelanoma skin cancer in moderate-risk subjects. A total of 2297 free-living subjects were enrolled; subjects resided in Arizona (median age, 63 years) and had a history of more than 10 actinic keratoses and at most 2 squamous cell carcinoma (SCC) or basal cell carcinoma (BCC) skin cancers. Subjects were randomly assigned to receive oral retinol (25,000 IU) or placebo supplementation daily for up to 5 years. The primary end points for the trial were time to first new SCC or BCC. During a median follow-up time of 3.8 years, we found that 526 subjects had a first new skin cancer. Comparing retinol-supplemented subjects with placebo-supplemented subjects showed a hazard ratio for first new SCC of 0.74 (95% confidence interval, 0.56-0.99; P = 0.04). The hazard ratio of first new BCC for the retinol-supplemented subjects compared with those receiving placebo was 1.06 (95% confidence interval, 0.86-1.32; P = 0.36). Potentially adverse symptoms that were judged to be associated with retinol were rare (approximately 1% higher in the retinol group than in the control group). Therefore, we concluded that daily supplementation with 25,000 IU of retinol was effective in preventing SCC, although it did not prevent BCC.

The retinoid skin cancer prevention (SKICAP) trials are a set of double-blind, randomized, placebo-controlled clinical trials. The SKICAP-actinic keratoses (AK) trial tests the hypothesis that daily supplementation of retinol (25,000 IU) for 5 years reduces the incidence of skin cancers in high-risk individuals, those with a history of greater than ten clinically or pathologically diagnosed AK and, at most, one prior pathologically confirmed cutaneous squamous cell carcinoma (SCC) or basal cell carcinoma (BCC). The SKICAP-SCC/BCC (S/B) trial tests the hypothesis that daily supplementation of retinol (25,000 IU) or 13-cis-retinoic acid (5 or 10 mg) for 3 years reduces skin cancer incidence in very high-risk individuals, those with a history of at least four pathologically confirmed SCCs or BCCs. Between 1984 and 1988, 2800 participants were enrolled at two clinics on the SKICAP-AK trial; and between 1985 and 1990, a total of 719 participants were enrolled at four clinics on the SKICAP-S/B trial. The initial recruitment strategy was referral by dermatologists, but low accrual necessitated the use of other strategies to achieve enrollment goals, which included involving additional clinics and using paid trial-specific advertisements in print and electronic media. Thirteen % of the SKICAP-AK participants and 36% of the SKICAP-S/B participants were enrolled through dermatologist referral, whereas paid advertisements resulted in enrollment of 87% of SKICAP-AK and 43% of SKICAP-S/B participants. A population-based skin cancer registry was used to identify and enroll the remaining 21% of the SKICAP-S/B participants.(ABSTRACT TRUNCATED AT 250 WORDS)

Affirmative action/equal opportunity policies have been around for some time; time enough for everyone concerned to take full advantage of the benefits provided by these policies. Some of America's successful Black scholars and health professionals who are the recipients of such good fortune brought about by these policies have made significant contributions toward the health and education of the nation and there is a need to continue the trend. The Black nursing student today must seize every opportunity; whether through Affirmative Action or otherwise to carry on the tradition of excellence among Black professionals. In spite of government mandates to enforce affirmative action and equal opportunity policies, the representation of Black nursing students in schools of nursing remains small. There seems to be some formidable barriers in the way, preventing these students from entering, remaining and graduating from nursing school. Deans and directors of nursing programs in Historically Black Universities and Colleges (HBCUs) are being called upon to assist Black nursing students to overcome these barriers and become successful nurses by utilizing Affirmative Action/Equal Opportunity policies.

We identify an abundant population of extreme emission line galaxies (EELGs) at redshift z~1.7 in the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) imaging from Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3). 69 EELG candidates are selected by the large contribution of exceptionally bright emission lines to their near-infrared broad-band magnitudes. Supported by spectroscopic confirmation of strong [OIII] emission lines -- with rest-frame equivalent widths ~1000\AA -- in the four candidates that have HST/WFC3 grism observations, we conclude that these objects are galaxies with 10^8 Msol in stellar mass, undergoing an enormous starburst phase with M_*/(dM_*/dt) of only ~15 Myr. These bursts may cause outflows that are strong enough to produce cored dark matter profiles in low-mass galaxies. The individual star formation rates and the co-moving number density (3.7x10^-4 Mpc^-3) can produce in ~4 Gyr much of the stellar mass density that is presently contained in 10^8-10^9 Msol dwarf galaxies. Therefore, our observations provide a strong indication that many or even most of the stars in present-day dwarf galaxies formed in strong, short-lived bursts, mostly at z>1., Comment: accepted for publication in ApJ; 10 pages; 6 figures; 1 table

1026 Background: Oxidative reactions have been implicated as important modulators of human health and the development of disease, including cancer. Studies have shown an increased oxidant burden in chronic obstructive pulmonary disease, a disease state in which there is increased risk of lung cancer. Our overall goal is to develop a safe, feasible clinical research approach using non-invasive methods of biomarker retrieval that will serve as a model for lung cancer chemoprevention studies. The primary study objective is to determine the effects of high green tea consumption (beverage and Polyphenon E [Mitsui-Norin Co., Ltd., Shizuoka, Japan]) on biomarkers of oxidative stress that are putative modulators of lung cancer risk, including 8-hydroxydeoxyguanosine (protein oxidation), F2-isoprostanes (lipid oxidation), nitric oxide and antioxidant enzymes. Secondary objectives are to measure modulation of lung carcinogenesis-related genes in exfoliated bronchoepithelial cells. Methods: We are conducting a 6-month randomized, controlled, double-blind trial of beverage green tea or Polyphenon E capsules or a control intervention (matching double placebo) in former smokers (FS) with a ≥30 pack year smoking history and an FEV1 ≤70%. Subjects are stratified by gender and inhaler use. Changes in oxidative damage are measured in exhaled breath condensate, blood and urine. Changes in gene expression of proliferative biomarkers (EGFR, PCNA, JUN, FOS, Ki-67) and apoptosis (bcl-2, caspase 3) are being assessed in induced sputum. Results: Recruitment and screening of subjects began 6/04. As of 12/05, 559 subjects have been phone screened for eligibility; of 99 eligible subjects, 54 were excluded by spirometry. 45 subjects have been enrolled and 25 have completed the study. No significant adverse events have been reported, including no liver toxicity. We have been able to extract RNA and measure gene expression in induced sputum. Conclusion: Six-month high tea consumption in FS with at least a moderate smoking history and FEV1 ≤70% is feasible and safe. Recruitment is continuing. Supported by U01-CA-101204. No significant financial relationships to disclose.

The 18O(p, α)15N reaction has been investigated in the energy range Ep = 72–935 keV. The three known resonances above Ep = 620 keV have been confirmed and four new resonances have been found below Ep = 340 keV. All observed resonances correspond to known compound states in 19F. Information on resonance energies, total widths and ωγ values is reported. The low-energy resonances are superimposed on a non-resonant reaction yield, which varies smoothly with beam energy and which exhibits pronounced α-particle angular distributions asymmetric around 90°. The explanation of these data requires either interferring amplitudes of broad resonances with differing parities or a direct (p, α) reaction mechanism. The investigated energy range corresponds to the important temperature range of T = (0.05–2.5) × 109 K. The energy averaged astrophysical reaction rates are compared with predictions.

The capture reaction3He(α,γ)7Be has been investigated in the energy range ofEc.m. =107 to 1,266 keV. The4He or3He beams of up to 300 μA particle current were incident on3He or4He gas targets, respectively. The gas target systems were all of the windowless and recirculating type. Excitation functions have been obtained with the use of an extended-static gas target, while the measurements ofγ-ray angular distributions involved a quasi-point supersonic jet system. The determination of absolute cross sections has been carried out with both types of gas target systems. Theγ-ray yields in the3He(α,γ)7Be reaction were detected using 80 cm3 Ge(Li) detectors. The data lead to a zero-energy intercept of the astrophysicalS(E) factor ofS(0)=0.30±0.03 keV-b. This result reduces the calculated solar neutrino rate by a factor of 1.76.

The review describes the current status of nuclear astrophysics, where special emphasis is given to primordial and stellar nucleosynthesis of the chemical elements. The laboratory approaches in obtaining relevant reaction rates are discussed. The authors also focus attention on those processes where new knowledge of nuclear physics may have important astrophysical consequences. The major burning phases in stars and some critical reactions are discussed. Finally, miscellaneous topics of current interest are described.

A search forγ-ray transitions within the broad groundstate of5Li has been carried out via the4He(p, γp*)4He reaction atEp(lab)=1.5−7.0 MeV. Differentially pumped gas targets of the extended and quasi-point types have been used. The results show that the set-up and detection techniques utilized are not sensitive enough to observe such intrastate transitions.

The use of monomeric and polymeric isocyanates in a wide variety of industries has been increasing. Little is known about the toxicity of polymeric isocyanates and the widely used 2,6-toluene diisocyanate (TDI) isomer. The pulmonary and sensory irritation of an aliphatic polyisocyanate (DES-N) based on hexamethylene diisocyanate (HDI) was studied in Swiss-Webster male mice during aerosol exposures in the range of 25 to 131 mg/m 3 . The sensory irritation of 2,6-TDI vapor was studied in the range of 0.37 to 7.6 mg/m 3 (0.05 to 1.1 ppm). The aerodynamic equivalent diameter and geometric standard deviation for the DES-N aerosol were 0.6 μm and 2.4, respectively. High-speed liquid chromatography was used to determine both free HDI in DES-N and HDI in the exposure chamber. Each exposure was for 3 hr during which the tidal volume pattern and respiratory rate of groups of four mice were recorded. Unlike the monomeric isocyanates, DES-N acted predominantly as a pulmonary irritant, evoking little sensory irritation. The concentration needed to reduce the respiratory rate 50% due to pulmonary irritation was 57.1 mg/m 3 . The LC50, determined by counting the number of deaths within the 24 hr period following a 4-hr exposure, was 91.2 mg/m 3 . In groups of animals killed 2 hr after the 4-hr exposure, the concentration of DES-N needed to increase lung weight by 50% was 45 mg/m 3 . Based on comparisons with another pulmonary irritant, nitrogen dioxide, the maximum concentration for DES-N permitted in industry should be 1 mg/m 3 with a time-weighted average for an 8-hr period of 0.5 mg/m 3 . From the concentration-response relationship due to sensory irritation for 2,6-TDI, the RD50 was determined to be 1.8 mg/m 3 (0.26 ppm) which is close to the value of 1.4 mg/m 3 (0.20 ppm) determined previously for 2,4-TDI. No pulmonary irritation was observed. For industrial applications the exposure limit for 2,4-TDI of 0.04 mg/m 3 (0.006 ppm) is also suggested as appropriate for the 2,6-TDI isomer.

Nuclear astrophysics is, in essence, a science that attempts to understand and explain the physical universe beyond the Earth by studying its smallest particles. "Cauldrons in the Cosmos", by Claus E. Rolfs and William S. Rodney, serves as a basic introduction to these endeavors. From the major discoveries in the field to a discussion of the makeup of stars to an explanation of standard lab techniques, this text provides students and scientists alike a thorough and fascinating survey of the accomplishments, goals, and methods of nuclear astrophysics. A classic in its field, "Cauldrons in the Cosmos" will surely remain an important reference in nuclear astrophysics for years to come.