Machine learning techniques to select Be star candidates. An application in the OGLE-IV Gaia south ecliptic pole field

Statistical pattern recognition methods have provided competitive solutions for variable star classification at a relatively low computational cost. In order to perform supervised classification, a set of features is proposed and used to train an automatic classification system. Quantities related to the magnitude density of the light curves and their Fourier coefficients have been chosen as features in previous studies. However, some of these features are not robust to the presence of outliers and the calculation of Fourier coefficients is computationally expensive for large data sets. We propose and evaluate the performance of a new robust set of features using supervised classifiers in order to look for new Be star candidates in the OGLE-IV Gaia south ecliptic pole field. We calculated the proposed set of features on six types of variable stars and on a set of Be star candidates reported in the literature. We evaluated the performance of these features using classification trees and random forests along with K-nearest neighbours, support vector machines, and gradient boosted trees methods. We tuned the classifiers with a 10-fold cross-validation and grid search. We validated the performance of the best classifier on a set of OGLE-IV light curves and applied this to find new Be star candidates. The random forest classifier outperformed the others. By using the random forest classifier and colour criteria we found 50 Be star candidates in the direction of the Gaia south ecliptic pole field, four of which have infrared colours consistent with Herbig Ae/Be stars. Supervised methods are very useful in order to obtain preliminary samples of variable stars extracted from large databases. As usual, the stars classified as Be stars candidates must be checked for the colours and spectroscopic characteristics expected for them

A Catalogue of Be Stars in the Direction of the Galactic Bulge

Detailed studies of Be stars in environments with different metallicities like the Magellanic Clouds or the Galactic bulge are necessary to understand the formation and evolution mechanisms of the circumstellar disks. However, a detailed study of Be stars in the direction of the bulge of our own galaxy has not been performed until now. We report the first systematic search for Be star candidates in the direction of the Galactic Bulge. We present the catalogue, give a brief description of the stellar variability seen, and show some light curve examples. We searched for stars matching specific criteria of magnitude, color and variability in the I band. Our search was conducted on the 48 OGLE II fields of the Galactic Bulge.This search has resulted in 29053 Be star candidates, 198 of them showing periodic light variations. Nearly 1500 stars in this final sample are almost certainly Be stars, providing an ideal sample for spectroscopic multiobject follow-up studies.Comment: Accepted for publication in A &

The influential effect of blending, bump, changing period and eclipsing Cepheids on the Leavitt law

The investigation of the non-linearity of the Leavitt law is a topic that began more than seven decades ago, when some of the studies in this field found that the Leavitt law has a break at about ten days. The goal of this work is to investigate a possible statistical cause of this non-linearity. By applying linear regressions to OGLE-II and OGLE-IV data, we find that, in order to obtain the Leavitt law by using linear regression, robust techniques to deal with influential points and/or outliers are needed instead of the ordinary least-squares regression traditionally used. In particular, by using $M$- and $MM$-regressions we establish firmly and without doubts the linearity of the Leavitt law in the Large Magellanic Cloud, without rejecting or excluding Cepheid data from the analysis. This implies that light curves of Cepheids suggesting blending, bumps, eclipses or period changes, do not affect the Leavitt law for this galaxy. For the SMC, including this kind of Cepheids, it is not possible to find an adequate model, probably due to the geometry of the galaxy. In that case, a possible influence of these stars could exist.Comment: 47 pages, 1 figure, 5 tables. Accepted for publication in Ap

La grafomotricidad en el proceso de aprendizaje de los ni?os de 5 a?os de la instituci?n t?cnica Sumapaz Sede Santa Clara

64 p. Recurso Electr?nico?Este proyecto atenido como objetivo principal, Establecer como el proceso de aprendizaje en los ni?os de 5 a?os, a trav?s diversas estrategias, desarrollando actividades que aporten a mejorar las destrezas de las manos, los dedos y su posici?n corporal para que tengan una buena motricidad al escribir y desarrollar las habilidades b?sicas para la iniciaci?n a la escritura, basada en el desarrollo de procesos motores b?sicos como: tipos y conservaciones de trazos, precisi?n en el uso de instrumentos y el desarrollo de habilidades grafomotoras. El t?rmino grafomotricidad en el nivel inicial es esencialmente un acto mot?rico que tiene por finalidad educar y corregir la ejecuci?n de los movimientos b?sicos que intervienen en la escritura. Estrada, R. (2006) aporta diciendo que la grafomotricidad es una fase previa a la escritura ya que supone el entrenamiento para la realizaci?n de movimientos b?sicos que forman parte de la correcta direccionalidad y trazado de las letras. Se puede afirmar que la grafomotricidad es una posibilidad que se plantea en este proyecto como una alternativa metodol?gica para facilitar el proceso de la escritura en los ni?os de la instituci?n educativa t?cnica sumapaz sede santa clara. Palabras claves: grafomotricidad, iniciaci?n en la escrituraThis project is considered as main objective, to establish learning strategies in the children of 5 years of the technical educational institution sumapaz seed Santa Clara headquarters, through diverse activities, developing exercises that contribute to improve the skills of the hands, the fingers and their body position To have a good motor skills in writing and develop the basic skills for initiation to writing, based on the development of basic motor processes such as types and conservations of strokes, precision in the use of instruments and the development of graphing skills. The term grafomotricidad in the initial level is essentially a motor act that has as purpose to educate and to correct the execution of the basic movements that take part in the writing. Estrada, R. (2006) contends that grafomotricidad is a pre-writing phase since it involves training for the realization of basic movements that are part of the correct directionality and layout of the letters. It is possible to affirm that the grafomotricidad is a possibility that arises in this project as a methodological alternative to facilitate the process of writing in the children of the technical educational institution sumapaz seed Santa Clara Keywords: grafomotricidad, initiation in the writin

Cobertura florestal secundária em pequenas propriedades rurais na Amazônia: implicações para a agricultura de corte e queima.

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Effect of universal MODS access on pulmonary tuberculosis treatment outcomes in new patients in Peru.

SETTING: Primary health care centres in Callao, Peru. OBJECTIVES: To evaluate the effect of universal access to the microscopic-observation drug susceptibility (MODS) assay on treatment outcomes in new and primary multidrug-resistant tuberculosis (MDR-TB) patients and on the process of drug susceptibility testing (DST). DESIGN: Retrospective review of tuberculosis (TB) registers and clinical records before (2007) and after (2009) the introduction of MODS in 2008. RESULTS: There were 281 patients in each cohort. Favourable treatment outcomes for 2007 (81%) and 2009 (77%) cohorts were similar. There was an increase in loss to follow-up (from 6% to 10%, P = 0.04) and a reduction in failure rates (from 4% to 0.4%, P = 0.01) in the 2009 compared with the 2007 cohort. In new MDR-TB cases (n = 22), a favourable treatment outcome was improved (from 46% to 82%, P = 0.183) in the 2009 cohort. DST coverage improved (from 24% to 74%, P < 0.001), and a significant reduction in time to diagnosis of drug-susceptible (from 118 to 33 days, P < 0.001) and MDR-TB (from 158 to 52 days, P =30.003) was observed in the 2009 cohort. CONCLUSION: Universal access to MODS increased DST coverage, reduced the time required to obtain DST results and was associated with reduced failure rates. MODS can make an important contribution to TB management and control in Peru

Diretrizes técnicas para a exploração de impacto reduzido em operações florestais de Terra Firme na Amazônia Brasileira.

Apresentação geral das diretrizes técnicas. Diretrizes para as atividades pré-exploratórias. diretrizes para as atividades de exploração florestal. Diretrizes para as atividades pós-exploratórias.bitstream/item/63188/1/Oriental-Doc64.pd

Emission-line stars discovered in the UKST H-alpha survey of the Large Magellanic Cloud; Part 1: Hot stars

We present new, accurate positions, spectral classifications, radial and rotational velocities, H-alpha fluxes, equivalent widths and B,V,I,R magnitudes for 579 hot emission-line stars (classes B0 - F9) in the Large Magellanic Cloud which include 469 new discoveries. Candidate emission line stars were discovered using a deep, high resolution H-alpha map of the central 25 deg2 of the LMC obtained by median stacking a dozen 2 hour H-alpha exposures taken with the UK Schmidt Telescope. Spectroscopic follow-up observations on the AAT, UKST, VLT, the SAAO 1.9m and the MSSSO 2.3m telescope have established the identity of these faint sources down to magnitude R~23 for H-alpha (4.5 x 10^-17 ergs cm^2 s^-1 Ang). Confirmed emission-line stars have been assigned an underlying spectral classification through cross-correlation against 131 absorption line template spectra covering the range O1 to F8. We confirm 111 previously identified emission line stars and 64 previously known variable stars with spectral types hotter than F8. The majority of hot stars identified (518 stars or 89%) are class B. Of all the hot emission-line stars in classes B-F, 130 or 22% are type B[e], characterised by the presence of forbidden emission lines such as [SII], [NII] and [OII]. We report on the physical location of these stars with reference to possible contamination from ambient HII emission. Along with flux calibration of the H-alpha emission we provide the first H-alpha luminosity function for selected sub-samples after correction for any possible nebula or ambient contamination. We find a moderate correlation between the intensity of H-alpha emission and the V magnitude of the central star based on SuperCOSMOS magnitudes and OGLE-II photometry where possible. Cool stars from classes G-S, with and without strong H-alpha emission, will be the focus of part 2 in this series.Comment: 24 pages (main paper) 36 figures, 6 tables; Appendix Tables: 22 pages, MNRAS, 201

Holographic energy density, dark energy sound speed, and tensions in cosmological parameters: H0H_0 and S8S_8

Interesting discrepancies in cosmological parameters are challenging the success of the $\Lambda$CDM model. Direct measurements of the Hubble constant $H_0$ using Cepheid variables and supernovae turn out to be higher than inferred from the Cosmic Microwave Background (CMB). Weak galaxy lensing surveys consistently report values of the strength of matter clustering $\sigma_8$ lower than values derived from the CMB in the context of $\Lambda$CDM. In this paper we address these discrepancies in cosmological parameters by considering Dark Energy (DE) as a fluid with evolving equation of state $w_{\mathrm{de}}(z)$, constant sound speed squared $\hat{c}_{\mathrm{s}}^{2}$, and vanishing anisotropic stress $\sigma$. Our $w_{\mathrm{de}}(z)$ is derived from the Holographic Principle and can consecutively exhibit radiation-like, matter-like, and DE-like behaviour, thus affecting the sound horizon and the comoving angular diameter distance, hence $H_0$. Here we show DE sound speed plays a part in the matter clustering behaviour through its effect on the evolution of the gravitational potential. We compute cosmological constraints using several data set combinations including primary CMB, CMB lensing, redshift-space-distortions, local distance-ladder, supernovae, and baryon acoustic oscillations. In our analysis we marginalise over $\hat{c}_{\mathrm{s}}^{2}$ and find $\hat{c}_{\mathrm{s}}^{2}=1$ is excluded at $\gtrsim 3\sigma$. For our baseline result including the whole data set we found $H_0$ and $\sigma_8$ in good agreement (within $\approx 2\sigma$) with low redshift probes. Our constraint for the baryon energy density $\omega_{\rm{b}}$ is however in $\approx 3\sigma$ tension with BBN constraints. We conclude evolving DE also having non-standard clustering properties [e.g., $\hat{c}_{\mathrm{s}}^{2}(z,k)$] might be relevant for the solution of current discrepancies in cosmological parameters.Comment: 28 pages, 12 figures, 3 tables. References adde

Searching for links between magnetic fields and stellar evolution. II. The evolution of magnetic fields as revealed by observations of Ap stars in open clusters and associations

The evolution of magnetic fields in Ap stars during the main sequence phase is presently mostly unconstrained by observation because of the difficulty of assigning accurate ages to known field Ap stars. We are carrying out a large survey of magnetic fields in cluster Ap stars with the goal of obtaining a sample of these stars with well-determined ages. In this paper we analyse the information available from the survey as it currently stands. We select from the available observational sample the stars that are probably (1) cluster or association members and (2) magnetic Ap stars. For the stars in this subsample we determine the fundamental parameters T_eff, log(L/L_o), and M/M_o. With these data and the cluster ages we assign both absolute age and fractional age (the fraction of the main sequence lifetime completed). For this purpose we have derived new bolometric corrections for Ap stars. Magnetic fields are present at the surfaces of Ap stars from the ZAMS to the TAMS. Statistically for the stars with M > 3 M_o the fields decline with advancing age approximately as expected from flux conservation together with increased stellar radius, or perhaps even faster than this rate, on a time scale of about 3 10^7 yr. In contrast, lower mass stars show no compelling evidence for field decrease even on a timescale of several times 10^8 yr. Study of magnetic cluster stars is now a powerful tool for obtaining constraints on evolution of Ap stars through the main sequence. Enlarging the sample of known cluster magnetic stars, and obtaining more precise RMS fields, will help to clarify the results obtained so far. Further field observations are in progress.Comment: Accepted by Astronomy & Astrophysic