Nuevos genotipos del nucleopoliedrovirus simple de Chrysodeixis chalcites (ChchSNPV), procedimiento para su producción y uso como agente de control biológico

Se describen tres nuevos genotipos del nucleopoliedrovirus de Chrysodeixis chalcites, ChchSNPV, purificados de un mismo aislado de las Islas Canarias. Cada uno de los genotipos tiene una actividad insecticida específica frente a larvas de ChchSNPV comparable a la de los insecticidas biológicos habituales. Además, la mezcla de los tres genotipos, particularmente en proporción 36:26:14, ya sea en forma de poliedros de un único genotipo o con viriones co-ocluidos de genotipos mezclados, es capaz de controlar las plagas de ChchSNPV en platanera de forma más eficiente que los insecticidas habituales, químicos o biológicos, siendo de los nucleopoliedrovirus más activos de los desarrollos como bioinsecticidas. Su uso como insecticida representa una tecnología segura para los vertebrados por ser específicos de invertebrados. Además, pueden producirse con facilidad y buen rendimiento por inoculación oral de larvas de C. chalcites con poliedros de ChchSNPV.Peer reviewedUniversidad Pública de Navarra, Consejo Superior de Investigaciones Científicas, Instituto canario de Investigaciones Agrarias, Instituto de EcologíaA1 Solicitud de patente con informe sobre el estado de la técnic

Nuevos genotipos del nucleopoliedrovirus simple de Chrysodeixis chalcites (ChchSNPV), procedimiento para su producción y uso como agente de control biológico

Se describen tres nuevos genotipos del nucleopoliedrovirus de Chrysodeixis chalcites, ChchSNPV, purificados de un mismo aislado de las Islas Canarias. Cada uno de los genotipos tiene una actividad insecticida específica frente a larvas de ChchSNPV comparable a la de los insecticidas biológicos habituales. Además, la mezcla de los tres genotipos, particularmente en proporción 36:26:14, ya sea en forma de poliedros de un único genotipo o con viriones co-ocluidos de genotipos mezclados, es capaz de controlar las plagas de ChchSNPV en platanera de forma más eficiente que los insecticidas habituales, químicos o biológicos, siendo de los nucleopoliedrovirus más activos de los desarrollos como bioinsecticidas. Su uso como insecticida representa una tecnología segura para los vertebrados por ser específicos de invertebrados. Además, pueden producirse con facilidad y buen rendimiento por inoculación oral de larvas de C. chalcites con poliedros de ChchSNPV.Peer reviewedUniversidad Pública de Navarra, Consejo Superior de Investigaciones Científicas, Instituto canario de Investigaciones Agrarias, Instituto de EcologíaA1 Solicitud de patente con informe sobre el estado de la técnic

Large-scale analysis of the SDSS-III DR8 photometric luminous galaxies angular correlation function

We analyse the large-scale angular correlation function (ACF) of the CMASS luminous galaxies (LGs), a photometric-redshift catalogue based on the Data Release 8 (DR8) of the Sloan Digital Sky Survey-III. This catalogue contains over $600 \, \, 000$ LGs in the range $0.45 \leq z \leq 0.65$, which was split into four redshift shells of constant width. First, we estimate the constraints on the redshift-space distortion (RSD) parameters $b\sigma_8$ and $f\sigma_8$, where $b$ is the galaxy bias, $f$ the growth rate and $\sigma_8$ is the normalization of the perturbations, finding that they vary appreciably among different redshift shells, in agreement with previous results using DR7 data. When assuming constant RSD parameters over the survey redshift range, we obtain $f\sigma_8 = 0.69 \pm 0.21$, which agrees at the $1.5\sigma$ level with Baryon Oscillation Spectroscopic Survey DR9 spectroscopic results. Next, we performed two cosmological analyses, where relevant parameters not fitted were kept fixed at their fiducial values. In the first analysis, we extracted the baryon acoustic oscillation peak position for the four redshift shells, and combined with the sound horizon scale from 7-year \textit{Wilkinson Microwave Anisotropy Probe} $(WMAP7)$ to produce the constraints $\Omega_{m}=0.249 \pm 0.031$ and $w=-0.885 \pm 0.145$. In the second analysis, we used the ACF full shape information to constrain cosmology using real data for the first time, finding $\Omega_{m} = 0.280 \pm 0.022$ and $f_b = \Omega_b/\Omega_m = 0.211 \pm 0.026$. These results are in good agreement with $WMAP7$ findings, showing that the ACF can be efficiently applied to constrain cosmology in future photometric galaxy surveys.Comment: MNRAS accepted. Minor corrections to match publish versio

Analisys of the fracture thoughness in the heat affected zone (HAZ) of one HSLA steel

Con la aportación original del trabajo experimental de investigación aquí realizado, se pretende asegurar que la tenacidad a la fractura KIC en la zona afectada por el calor (ZAC) del acero USITEN 355 0,5 Ni grado I, produce un CTOD (?) (Crack Tip Opening Displacement) con valores dentro de la norma, haciendo compatible el acero con el procedimiento de soldadura utilizado y la energía calorífica aportada de 2 kJ /mm, comprobando que el mecanismo de frenado del tamaño de grano llevado a cabo por los microaleantes (V, Nb, Al) del metal base funcionan conforme lo previsto. Además, se intenta asegurar, en la medida de lo posible, una correlación entre los parámetros de soldadura y los resultados obtenidos en los ensayos de fractura, de tal forma que, si los resultados obtenidos en los ensayos no fueran satisfactorios, se pudiese aplicar la solución adecuada en el soldeo para que los parámetros que regulan los ensayos de fractura sean aceptables. El trabajo aquí desarrollado es útil como guía y referencia para futuros trabajos de investigación de mecánica de la fractura en aceros microaleados

Redshift measurement and spectral classification for eBOSS galaxies with the redmonster software

We describe the redmonster automated redshift measurement and spectral classification software designed for the extended Baryon Oscillation Spectroscopic Survey (eBOSS) of the Sloan Digital Sky Survey IV (SDSS-IV). We describe the algorithms, the template standard and requirements, and the newly developed galaxy templates to be used on eBOSS spectra. We present results from testing on early data from eBOSS, where we have found a 90.5% automated redshift and spectral classification success rate for the luminous red galaxy sample (redshifts 0.6 ≲ z ≲ 1.0). The redmonster performance meets the eBOSS cosmology requirements for redshift classification and catastrophic failures and represents a significant improvement over the previous pipeline. We describe the empirical processes used to determine the optimum number of additive polynomial terms in our models and an acceptable ΔXr2 threshold for declaring statistical confidence. Statistical errors on redshift measurement due to photon shot noise are assessed, and we find typical values of a few tens of km s-1. An investigation of redshift differences in repeat observations scaled by error estimates yields a distribution with a Gaussian mean and standard deviation of μ ∼ 0.01 and σ ∼ 0.65, respectively, suggesting the reported statistical redshift uncertainties are over-estimated by ∼54%. We assess the effects of object magnitude, signal-to-noise ratio, fiber number, and fiber head location on the pipeline's redshift success rate. Finally, we describe directions of ongoing development.Publisher PDFPeer reviewe

Spectral variability of a sample of extreme variability quasars and implications for the MgII broad-line region

We present new Gemini/GMOS optical spectroscopy of 16 extreme variability quasars (EVQs) that dimmed by more than 1.5 mag in the g band between the Sloan Digital Sky Survey (SDSS) and the Dark Energy Survey epochs (separated by a few years in the quasar rest frame). These EVQs are selected from quasars in the SDSS Stripe 82 region, covering a redshift range of 0.5 < z < 2.1. Nearly half of these EVQs brightened significantly (by more than 0.5 mag in the g band) in a few years after reaching their previous faintest state, and some EVQs showed rapid (non-blazar) variations of greater than 1-2 mag on time-scales of only months. To increase sample statistics, we use a supplemental sample of 33 EVQs with multi-epoch spectra from SDSS that cover the broad Mg II λ2798 line. Leveraging on the large dynamic range in continuum variability between the multi-epoch spectra, we explore the associated variations in the broad Mg II line, whose variability properties have not been well studied before. The broad Mg II flux varies in the same direction as the continuum flux, albeit with a smaller amplitude, which indicates at least some portion of Mg II is reverberating to continuum changes. However, the full width at half-maximum (FWHM) of Mg II does not vary accordingly as continuum changes for most objects in the sample, in contrast to the case of the broad Balmer lines. Using the width of broad Mg II to estimate the black hole mass with single epoch spectra therefore introduces a luminosity-dependent bias.QY and YS acknowledge support from an Alfred P. Sloan Research Fellowship (YS) and NSF grant AST1715579. We thank Patrick Hall, Tamara Davis, Shu Wang, and Hengxiao Guo for useful discussions and suggestions. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ao Carlos ˜ Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, ` Conselho Nacional de Desenvolvimento Cient´ıfico e Tecnologico ´ and the Ministerio da Ci ´ encia, Tecnologia e Inovac ˆ ¸ao, the Deutsche ˜ Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey

Primordial non-Gaussianity with Angular correlation function: Integral constraint and validation for DES

Local primordial non-Gaussianity (PNG) is a promising observable of the underlying physics of inflation, characterised by $f_{\rm NL}^{\rm loc}$. We present the methodology to measure $f_{\rm NL}^{\rm loc}$ from the Dark Energy Survey (DES) data using the 2-point angular correlation function (ACF) with scale-dependent bias. One of the focuses of the work is the integral constraint. This condition appears when estimating the mean number density of galaxies from the data and is key in obtaining unbiased $f_{\rm NL}^{\rm loc}$ constraints. The methods are analysed for two types of simulations: $\sim 246$ GOLIAT-PNG N-body small area simulations with $f_{\rm NL}$ equal to -100 and 100, and 1952 Gaussian ICE-COLA mocks with $f_{\rm NL}=0$ that follow the DES angular and redshift distribution. We use the ensemble of GOLIAT-PNG mocks to show the importance of the integral constraint when measuring PNG, where we recover the fiducial values of $f_{\rm NL}$ within the $1\sigma$ when including the integral constraint. In contrast, we found a bias of $\Delta f_{\rm NL}\sim 100$ when not including it. For a DES-like scenario, we forecast a bias of $\Delta f_{\rm NL} \sim 23$, equivalent to $1.8\sigma$, when not using the IC for a fiducial value of $f_{\rm NL}=100$. We use the ICE-COLA mocks to validate our analysis in a realistic DES-like setup finding it robust to different analysis choices: best-fit estimator, the effect of IC, BAO damping, covariance, and scale choices. We forecast a measurement of $f_{\rm NL}$ within $\sigma(f_{\rm NL})=31$ when using the DES-Y3 BAO sample, with the ACF in the $1\ {\rm deg}<\theta<20\ {\rm deg}$ range.Comment: Version after MNRAS reviewer comments. Improved discussion in Section 7. 16 pages, 11 figure