A nearby GRB host prototype for z~7 Lyman-break galaxies: Spitzer-IRS and X-shooter spectroscopy of the host galaxy of GRB031203

Gamma-ray burst (GRB) host galaxies have been studied extensively in optical photometry and spectroscopy. Here we present the first mid-infrared spectrum of a GRB host, HG031203. It is one of the nearest GRB hosts at z=0.1055, allowing both low and high-resolution spectroscopy with Spitzer-IRS. Medium resolution UV-to-K-band spectroscopy with the X-shooter spectrograph on the VLT is also presented, along with Spitzer IRAC and MIPS photometry, as well as radio and sub-mm observations. These data allow us to construct a UV-to-radio spectral energy distribution with almost complete spectroscopic coverage from 0.3-35 micron of a GRB host galaxy for the first time, potentially valuable as a template for future model comparisons. The IRS spectra show strong, high-ionisation fine structure line emission indicative of a hard radiation field in the galaxy, suggestive of strong ongoing star-formation and a very young stellar population. The selection of HG031203 via the presence of a GRB suggests that it might be a useful analogue of very young star-forming galaxies in the early universe, and hints that local BCDs may be used as more reliable analogues of star-formation in the early universe than typical local starbursts. We look at the current debate on the ages of the dominant stellar populations in z~7 and z~8 galaxies in this context. The nebular line emission is so strong in HG031203, that at z~7, it can reproduce the spectral energy distributions of z-band dropout galaxies with elevated IRAC 3.6 and 4.5 micron fluxes without the need to invoke a 4000A break.Comment: Published in ApJ. 9 pages, 6 figures, emulateapj styl

Filogenia del virus linfotrópico humano htlv-1 en sudamérica

Se postula que el HTLV-I salió de África hacia otras áreas del mundo incluyendo Suramérica; sin embargo, actualmente no existe un consenso sobre las rutas de introducción ni el periodo en que ocurrieron

Genotype and environment interaction in Colombian Holstein cattle

The existence of Genotype-Environment Interactions among four regions of Colombia was investigated. The information was obtained from records of Holstein cattle in Cundinamarca (C), Valle del Cauca(V), Antioquia (A) and Nariño (N). A mixed models multivariate analysis methodology, applied to an animal model for repeated measures was used. Variance components were estimated by Derivative Free Restricted Maximum Likelihood algorithm (DFREML). Contemporary group (Herd-year) and genetic group of the sires (origin-year of birth) were fixed effects, and the genetic additive, permanent environment and temporary environment were included as random effects. Production records (n = 69464) of 25 608 daughters of 594 sires were used. Genetic correlation coefficients of milk production between regions were 0.70, 0.83, 0.73, 0.95, 0.97 and 0.99 for C-V, C-A, C-N, V-A, V-N and A-N, respectively. Different genetic, permanent environment and residual variances among areas were observed, but heritabilities and repetibilities were similar. Genotype and Environment Interaction exists, mainly between Cundinamarca and the other three regions

Changes of salivary biomarkers under different storage conditions : Effects of temperature and length of storage

Introduction: In this report, we aimed to examine the stability of various analytes in saliva under different storage conditions. Materials and methods: Alpha-amylase (AMY), cholinesterase (CHE), lipase (Lip), total esterase (TEA), creatine kinase (CK), aspartate aminotransferase (AST), lactate dehydrogenase (LD), lactate (Lact), adenosine deaminase (ADA), Trolox equivalent antioxidant capacity (TEAC), ferric reducing ability (FRAS), cupric reducing antioxidant capacity (CUPRAC), uric acid (UA), catalase (CAT), advanced oxidation protein products (AOPP) and hydrogen peroxide (H O) were colorimetrically measured in saliva obtained by passive drool from 12 healthy voluntary donors at baseline and after 3, 6, 24, 72 hours, 7 and 14 days at room temperature (RT) and 4 ºC, and after 14 days, 1, 3 and 6 months at - 20 ºC and - 80 ºC. Results: At RT, changes appeared at 6 hours for TEA and H O; 24 hours for Lip, CK, ADA and CUPRAC; and 72 hours for LD, Lact, FRAS, UA and AOPP. At 4 ºC changes were observed after 6 hours for TEA and H O; 24 hours for Lip and CUPRAC; 72 hours for CK; and 7 days for LD, FRAS and UA. At - 20 ºC changes appeared after 14 days for AST, Lip, CK and LD; and 3 months for TEA and H O. At - 80 ºC observed changes were after 3 months for TEA and H O. Conclusions: In short-term storage, the analytes were more stable at 4 ºC than at room temperature, whereas in long-term storage they were more stable at -80 ºC than at - 20 ºC

Standard and Embedded Solitons in Nematic Optical Fibers

A model for a non-Kerr cylindrical nematic fiber is presented. We use the multiple scales method to show the possibility of constructing different kinds of wavepackets of transverse magnetic (TM) modes propagating through the fiber. This procedure allows us to generate different hierarchies of nonlinear partial differential equations (PDEs) which describe the propagation of optical pulses along the fiber. We go beyond the usual weakly nonlinear limit of a Kerr medium and derive an extended Nonlinear Schrodinger equation (eNLS) with a third order derivative nonlinearity, governing the dynamics for the amplitude of the wavepacket. In this derivation the dispersion, self-focussing and diffraction in the nematic are taken into account. Although the resulting nonlinear $PDE$ may be reduced to the modified Korteweg de Vries equation (mKdV), it also has additional complex solutions which include two-parameter families of bright and dark complex solitons. We show analytically that under certain conditions, the bright solitons are actually double embedded solitons. We explain why these solitons do not radiate at all, even though their wavenumbers are contained in the linear spectrum of the system. Finally, we close the paper by making comments on the advantages as well as the limitations of our approach, and on further generalizations of the model and method presented.Comment: "Physical Review E, in press

Caracterización genética de las razas Hartón del Valle, Angus, Brangus, Holstein y Senepol en Colombia, usando 10 marcadores microsatélites

ABSTRACT: The objective of this paper is to establish a genetic characterization of the Senepol (S, n=49), Holstein (H, n= 60), Hartón del Valle (HV, n=60), Angus (A, n=61) and Brangus (Br, n=60) cattle breeds in Colombia, by using the following microsatellite markers: SPS115, INRA64, ETH225, ETH10, BM1824, INRA37, TGLA122, TGLA126, INRA32, and BM2113. A total of 142 alleles were obtained for ten analyzed loci, considering the five cattle breeds as a whole. The number of alleles per locus ranged from 9 (INRA64 and 1824) to 22 (TGLA122). The expected heterozygosity was between 0.79 (INRA32) and 0.90 (INRA37) in all the cattle breeds, respectively; and medium heterozygosity was 0.84. The average number of alleles per breed varied from 9.2 in the Senepol breed to 10.3 in the Holstein breed. The expected heterozygosity range varied from 0.75 in the Hartón del Valle breed and 0.82 in the Holstein breed, with an average of 0.79. Hardy Wienberg disequilibrium was observed (p>0.05) when the populations were analyzed with all the markers. All the populations presented a heterozygote deficit, which could be the result of a strong endogamy tendency within all the herds. The markers used in this study allowed a genetic characterization of the analyzed populations. The microsatellites panel in the Hartón del Valle breed should be increased in order to increase the reliability value. Microsatellite panels could solve parenthood cases for the remainder breeds.RESUMEN: El objetivo de este trabajo fue caracterizar genéticamente las razas bovinas Senepol (S, n=49), Holstein (H, n= 60), Hartón del Valle (HV, n=60), Angus (A, n=61) y Brangus (Br, n=60) en Colombia, con los marcadores microsatélites SPS115, INRA64, ETH225, ETH10, BM1824, INRA37, TGLA122, TGLA126, INRA32 y BM2113. En total, 142 alelos fueron encontrados en los diez loci analizados, considerando las cinco razas como un todo. El número de alelos por locus estuvo entre 9 (INRA64 y BM1824) y 22 (TGLA122). La Heterocigosidad esperada a través de todas las razas varió entre 0.79 (INRA32) y 0,90 (INRA37) y heterocigosidad media esperada de 0.84. El número promedio de alelos por raza varió de 9.2 en la raza S a 10.3 en la raza H. El rango de la Heterocigosidad esperada entre las razas varió entre 0.75 en la raza HV y 0.82 en la raza H, con una media de 0.79. Al analizar las poblaciones con el total de marcadores, todas se encontraron en desequilibrio de Hardy Weinberg (p>0.05). Todas las poblaciones presentaron un déficit de heterocigotos, para todas las poblaciones, lo que podría ser el resultado de la fuerte tendencia a la endogamia dentro de los diferentes hatos. Los resultados indicaron que los marcadores utilizados en este estudio permitieron caracterizar genéticamente las poblaciones analizadas. En el caso de la Raza HV, se debe aumentar el panel de microsatélites para aumentar el valor de confiabilidad. Para las demás razas el panel de microsatélites permitiría resolver casos de filiación

Detection of an optical transient following the 13 March 2000 short/hard gamma-ray burst

We imaged the error box of a gamma-ray burst of the short (0.5 s), hard type (GRB 000313), with the BOOTES-1 experiment in southern Spain, starting 4 min after the gamma-ray event, in the I-band. A bright optical transient (OT 000313) with I = 9.4 +/- 0.1 was found in the BOOTES-1 image, close to the error box (3-sigma) provided by BATSE. Late time VRIK'-band deep observations failed to reveal an underlying host galaxy. If the OT 000313 is related to the short, hard GRB 000313, this would be the first optical counterpart ever found for this kind of events (all counterparts to date have been found for bursts of the long, soft type). The fact that only prompt optical emission has been detected (but no afterglow emission at all, as supported by theoretical models) might explain why no optical counterparts have ever been found for short, hard GRBs.This fact suggests that most short bursts might occur in a low-density medium and favours the models that relate them to binary mergers in very low-density enviroments.Comment: Revised version. Accepted for publication in Astronomy and Astrophysics Letters, 5 pages, 3 figure

Juvenile xanthogranuloma. Presentation of a clinical case and review of the topic

El Xantogranuloma Juvenil (XGJ) es un tumor benigno de piel que afecta principalmente la población infantil, más comúnmente durante el primer año de edad. Hace parte del grupo de las Histiocitosis no X y tienden a ser autorresolutivas. Ocasionalmente puede comprometer otros órganos, siendo el compromiso ocular el más frecuente con riesgo de llevar hasta la ceguera. Los autores presentan un caso en una niña de 2 meses con lesiones múltiples y hacen una revisión del tema. (Camargo AM, Rojas RF, Serrano JC. Xantogranuloma juvenil. Presentación de un caso clínico y revisión del tema. MedUNAB 2003; 6:155-9)Juvenile Xanthogranuloma (JXG) is a benign skin tumor that mainly affects children, more commonly during the first year of age. It is part of the non-X Histiocytosis group and tends to be self-resolving. Occasionally it can compromise other organs, being the ocular compromise the most frequent with risk of even blindness. The authors present a case of a 2-month-old girl with multiple injuries and review the subject. (Camargo AM, Rojas RF, Serrano JC. Juvenile xanthogranuloma. Presentation of a clinical case and review of the topic. MedUNAB 2003; 6:155-9

A multi-colour study of the dark GRB 000210 host galaxy and its environment

We present UBVRIZJsHKs broad band photometry of the host galaxy of the dark gamma-ray burst (GRB) of February 10, 2000. These observations represent the most exhaustive photometry given to date of any GRB host galaxy. A grid of spectral templates have been fitted to the Spectral Energy Distribution (SED) of the host. The derived photometric redshift is z=0.842^+0.054_-0.042, which is in excellent agreement with the spectroscopic redshift (z=0.8463+/-0.0002) proposed by Piro et al. (2002) based on a single emission line. Furthermore, we have determined the photometric redshift of all the galaxies in an area of 6'x6' around the host galaxy, in order to check for their overdensity in the environment of the host. We find that the GRB 000210 host galaxy is a subluminous galaxy (L ~ 0.5+/-0.2 L*), with no companions above our detection threshold of 0.18+/-0.06 L*. Based on the restframe ultraviolet flux a star formation rate of 2.1+/-0.2 Solar Masses per year is estimated. The best fit to the SED is obtained for a starburst template with an age of 0.181^+0.037_-0.026 Gyr and a very low extinction (Av~0). We discuss the implications of the inferred low value of Av and the age of the dominant stellar population for the non detection of the GRB 000210 optical afterglow.Comment: 10 pages with 4 encapsulated PostScript figures included. Accepted for publication in Astronomy & Astrophysic