Andes Virus and First Case Report of Bermejo Virus Causing Fatal Pulmonary Syndrome

Two suspected hantavirus pulmonary syndrome (HPS) cases from Bolivia were confirmed by enzyme-linked immunosorbent assay. (ELISA)-ANDES was performed using N-Andes recombinant antigen serology in May and July 2000. Clot RNAs from the two patients were subjected to reverse transcription–polymerase chain reaction (PCR) amplification and sequencing. We describe two characterized cases of HPS. One was caused by infection with Bermejo virus and the other with Andes Nort viral lineage, both previously obtained from Oligoryzomys species. This is the first report of molecular identification of a human hantavirus associated with Bermejo virus

A New Digital Preoperative Planning Method for Total Hip Arthroplasties

Preoperative templating is an important part of a THA. The ability to accurately determine magnification of the hip on the radiograph and apply identical magnification to the radiograph and template will improve accuracy of preoperative templating of THA. We designed a templating method using a new way of determining the hip magnification with a linear relationship between magnification of the hip and the reference object on top of the pubis symphysis; the relationship was determined on 50 radiographs. We then compared our method with two other templating methods: an analog method assuming an average hip magnification of 15% and a digital method determining the hip magnification with a one-to-one relationship between the reference object and the hip. All methods were reproducible. Uniform undersizing occurred when templating with the digital method based on the one-to-one relationship; the analog method best predicted the implanted prosthesis size, closely followed by our new digital templating method; the new method will be particularly applicable for preoperative THA when analog methods are replaced by digital methods

ANÁLISE ASSISTENCIAL da UNIDADE DE CUIDADOS PALIAT IVOS ONCOLÓGICOS EM UM HOSPITAL PART ICULAR NA CIDADE DE MONTEVIDÉU

“The Palliative Care Unit is defined as an organization of health professionals providing multidisciplinary care through a broad spectrum of forms of assistance which necessarily includes hospitalization in specific beds. The UCP must meet functional, structural and organizational requirements that ensure adequate conditions of quality, safety and efficiency to perform this activity “(1). The overall objective is to analyze the welfare aspect of the Oncology Palliative Care Unit of a Hospital located in Montevideo in its first year of operation. The methodology performed is a descriptive, retrospective cross-sectional study.The results show that 379 users were treated and 2487 consultations were performed in sanatorium, clinic and user´s home. Most users served are males with an average age of 76, being derived mostly by oncologists. The elastomeric infusor was used in 85 of them. 301 died, the majority of deaths occurring in the Hospi Saunders II. In regards to psychological care, its risk and need was assessed for 117 users and their families. A letter of condolence was sent to 57 families, and 13 mourning families were assisted. The Ministry of Public Health considers that 921 users could receive palliative care in our institution. 379 users were helped in a year by this unit. This is an important quantity; comparing data concerning other palliative care units in Uruguay.“La UCP (Unidad de Cuidados Paliativos) se define como una organización de profesionales sanitarios, que ofrece atención multidisciplinaria mediante un amplio espectro de modalidades de asistencia que incluye necesariamente la hospitalización en camas específicas. Para realizar esta actividad la UCP debe cumplir unos requisitos funcionales, estructurales y organizativos, que garantizan las condiciones adecuadas de calidad,seguridad y eficiencia”(1). El objetivo general es analizar el aspecto asistencial de una Unidad de Cuidados Paliativos Oncológicos de la ciudad de Montevideo en su primer año defuncionamiento. Para esto se realizó un estudio descriptivo, retrospectivo de corte transversal. Los resultados arrojaron que se atendieron 379 usuarios, realizándose 2487 consultas distribuidas en sanatorio, policlínica y domicilio. La mayoría de los usuarios atendidos son de sexo masculino con una edad media de 76 años, siendo derivados casi todos por médicos oncólogos. Fallecieron 301 de los usuarios, muchos de ellos en elHospi Saunders II. Se utilizó el recurso del infusor elastomérico en 85 de ellos. En relación a la asistencia psicológica se evaluó el riesgo y la necesidad en 117 usuarios y sus familias,enviándose a 57 familias cartas de condolencias. Se asistió en duelo a 13 familias. El Ministerio de Salud Pública considera que 921 usuarios serían pasibles de cuidados paliativos en esta mutualista. En un año fueron captados por esta unidad 379 usuarios. Este es un número importante comparando los datos con unidades de cuidados paliativos referentes en Uruguay.“A UCP (Unidade de Cuidados Paliativos) é definida como uma organização de profissionais de saúde que prestam atendimento multidisciplinar através de um amplo espectro de formas de assistência que necessariamente inclui camas de hospitalização específicas. A UCP deve atender aos requisitos funcionais, estruturais e organizacionais que assegurem condições adequadas de qualidade, segurança e eficiência para realizar esta atividade “(1). O objetivo geral é analisar o aspecto do bem-estar de Oncologia Palliative Care Unit da Associação Espanhola de Montevidéu, em seu primeiro ano de operação. Metodologia: um estudo descritivo transversal, retrospectivo foi realizado. 379 usuários atendidos, realizando consultas distribuídas em 2.487 sanatório, clínica e em casa. A maioria dos usuários atendidos são do sexo masculino, com idade média de 76, sendo derivada principalmente por médicos oncologistas. O uso de infusor elastomérica em 85 usuários usada, 301 morreram ea maioria das mortes no Hospice Saunders II. No que diz respeito ao risco de atendimento psicológico e da necessidade de 117 usuários e suas famílias, o envio de uma carta de condolências 57 famílias, com a assistência de 13 famílias enlutadas que foram avaliados. O Ministério da Saúde considera 921 usuários seria susceptível de nossa mútua paliativos, cuidados em um ano foram apanhados por esta unidade 379 usuários. Este é um número importante comparar dados relativos às unidades de cuidados paliativos no Uruguai

What is the closest black hole to the Sun?

We examine the distance of the two galactic microquasars GRO J1655-40 and A0620-00, which are potentially the two closest black holes to the Sun. We aim to provide a picture as wide and complete as possible of the problem of measuring the distance of microquasars in our Galaxy. The purpose of this work is to fairly and critically review in great detail every distance method used for these two microquasars in order to show that the distances of probably all microquasars in our galaxy are much more uncertain than currently admitted. Moreover, we show that many confirmations of quantitative results are often entangled and rely on very uncertain measurements. We also present a new determination of the maximum distance of GRO J1655-40 using red clump giant stars, and show that it confirms our earlier result of a distance less than 2 kpc instead of 3.2 kpc. Since it then becomes more likely that GRO J1655-40 could originate from the stellar cluster NGC 6242, located at 1.0 kpc, we review the distance estimations of A0620-00, which is so far the closest black hole with an average distance of about 1.0 kpc. We show that the distance methods used for A0620-00 are also problematic. Finally, we present a new analysis of spectroscopic and astrometric archival data on this microquasar, and apply the maximum-distance method of Foellmi et al. (2006). It appears that A0620-00 could indeed be even closer to the Sun than currently estimated, and consequently would be the closest known black hole to the Sun.Comment: Accepted for publication in New Astronomy. 27 pages, 7 figures, Added new column in Table 1. Corrected definition of mass ratio in Equ 1

An enigmatic long-lasting γ-ray burst not accompanied by a bright supernova

Gamma-ray bursts (GRBs) are short, intense flashes of soft γ-rays coming from the distant Universe. Long-duration GRBs (those lasting more than ~2s) are believed to originate from the deaths of massive stars, mainly on the basis of a handful of solid associations between GRBs and supernovae. GRB 060614, one of the closest GRBs discovered, consisted of a 5-s hard spike followed by softer, brighter emission that lasted for ~100s (refs 8, 9). Here we report deep optical observations of GRB 060614 showing no emerging supernova with absolute visual magnitude brighter than MV=-13.7. Any supernova associated with GRB 060614 was therefore at least 100 times fainter, at optical wavelengths, than the other supernovae associated with GRBs. This demonstrates that some long-lasting GRBs can either be associated with a very faint supernova or produced by different phenomena.Fil: Della Valle, M.. Osservatorio Astrofisico di Arcetri; ItaliaFil: Chincarini, G.. Osservatorio Astronomico di Brera; ItaliaFil: Panagia, N.. Space Telescope Science Institute; Estados UnidosFil: Tagliaferri, G.. Osservatorio Astronomico di Brera; ItaliaFil: Malesani, D.. International School for Advanced Studies; ItaliaFil: Testa, V.. Osservatorio Astronomico di Roma; ItaliaFil: Fugazza, D.. Osservatorio Astronomico di Brera; ItaliaFil: Campana, S.. Osservatorio Astronomico di Brera; ItaliaFil: Covino, S.. Osservatorio Astronomico di Brera; ItaliaFil: Mangano, V.. Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo; ItaliaFil: Antonelli, L. A.. Osservatorio Astronomico di Roma; ItaliaFil: D'Avanzo, P.. Osservatorio Astronomico di Brera; ItaliaFil: Hurley, K.. University Of California Berkeley; Estados UnidosFil: Mirabel Miquele, Igor Felix. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Pellizza González, Leonardo Javier. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Piranomonte, S.. Osservatorio Astronomico di Roma; ItaliaFil: Stella, L.. Osservatorio Astronomico di Roma; Itali

The secrets of T Pyxidis II. A recurrent nova that will not become a SN Ia

By various methods, we obtained L$_{disk}$ $\sim$ 70 L$_{\odot}$ and $\dot{M}$ $\sim$1.1 $\times$ 10$^{-8}$ M$_{\odot}$yr$^{-1}$. These values were about twice as high in the pre-1966-outburst epoch. This allowed the first direct estimate of the total mass accreted before outburst, M$_{accr}$=$\dot{M}_{pre-OB}$ $\cdot \Delta$t, and its comparison with the critical ignition mass M$_{ign}$. We found M$_{accr}$ and M$_{ign}$ to be in perfect agreement (with a value close to 5 $\times$ 10$^{-7}$M$_{\odot}$) for M$_1$ $\sim$ 1.37 M$_{\odot}$, which provides a confirmation of the thermonuclear runaway theory. The comparison of the observed parameters of the eruption phase, with the corresponding values in the grid of models by Yaron and collaborators, provides satisfactory agreement for values of M$_1$ close to 1.35 M$_{\odot}$ and log$\dot{M}$ between -8.0 and -7.0, but the observed value of the decay time t$_3$ is higher than expected. The long duration of the optically thick phase during the recorded outbursts of T Pyx, a spectroscopic behavior typical of classical novae, and the persistence of P Cyg profiles, constrains the ejected mass M$_{ign}$ to within 10$^{-5}$ - 10$^{-4}$ M$_{\odot}$. Therefore, T Pyx ejects far more material than it has accreted, and the mass of the white dwarf will not increase to the Chandrasekhar limit as generally believed in recurrent novae. A detailed study based on the UV data excludes the possibility that T Pyx belongs to the class of the supersoft X-ray sources, as has been postulated. XMM-NEWTON observations have revealed a weak, hard source and confirmed this interpretation

BlackCAT: A catalogue of stellar-mass black holes in X-ray transients

During the last ~50 years, the population of black hole candidates in X-ray binaries has increased considerably with 59 Galactic objects detected in transient low-mass X-ray binaries, plus a few in persistent systems (including ~5 extragalactic binaries). We collect near-infrared, optical and X-ray information spread over hundreds of references in order to study the population of black holes in X-ray transients as a whole. We present the most updated catalogue of black hole transients, which contains X-ray, optical and near-infrared observations together with their astrometric and dynamical properties. It provides new useful information in both statistical and observational parameters providing a thorough and complete overview of the black hole population in the Milky Way. Analysing the distances and spatial distribution of the observed systems, we estimate a total population of ~1300 Galactic black hole transients. This means that we have already discovered less than ~5% of the total Galactic distribution. The complete version of this catalogue will be continuously updated online and in the Virtual Observatory, including finding charts and data in other wavelengths.Comment: http://www.astro.puc.cl/BlackCAT - Accepted for publication in Astronomy & Astrophysics. 20 pages, 8 figures, 5 Table

Early-type galaxies with core collapse supernovae

It is widely accepted that the progenitors of core collapse SNe are young massive stars and therefore their host galaxies are mostly spiral or irregular galaxies dominated by a young stellar population. Surprisingly, among morphologically classified hosts of core collapse SNe, we find 22 cases where the host has been classified as an Elliptical or S0 galaxy. To clarify this apparent contradiction, we carry out a detailed morphological study and an extensive literature search for additional information on the sample objects. Our results are as follows: 1. Of 22 "early type" objects, 17 are in fact misclassified spiral galaxies, one is a misclassified irregular, and one is a misclassified ring galaxy. 2. Of the 3 objects maintaining the early type classification, one (NGC2768) is a suspected merger remnant, another (NGC4589) is definitely a merger, and the third (NGC2274) is in close interaction. The presence of some amount of young stellar population in these galaxies is therefore not unexpected. These results confirm the presence of a limited, but significant, number of core collapse SNe in galaxies generally classified of early type. In all cases, anyway, there are independent indicators of the presence in host galaxies of recent star formation due to merging or gravitational interaction.Comment: 12 pages, 1 figure, 1 table, accepted for publication in A&

BVRI Light Curves for 29 Type Ia Supernovae

BVRI light curves are presented for 27 Type Ia supernovae discovered during the course of the Calan/Tololo Survey and for two other SNe Ia observed during the same period. Estimates of the maximum light magnitudes in the B, V, and I bands and the initial decline rate parameter m15(B) are also given.Comment: 17 pages, figures and tables are not included (contact first author if needed), to appear in the Astronomical Journa

Star Formation History up to z = 7.4: Implications for Gamma-Ray Bursts and the Cosmic Metallicity Evolution

The current Swift sample of gamma-ray bursts (GRBs) with measured redshifts allows to test the assumption that GRBs trace the star formation in the Universe. Some authors have claimed that the rate of GRBs increases with cosmic redshift faster than the star formation rate, whose cause is not known yet. In this paper, I investigate the possibility for interpreting the observed discrepancy between the GRB rate history and the star formation rate history by the cosmic metallicity evolution, motivated by the observation that the cosmic metallicity evolves with redshift and GRBs prefer to occur in low metallicity galaxies. First, I derive a star formation history up to redshift z=7.4 from an updated sample of star formation rate densities obtained by adding the new UV measurements of Bouwens et al. and the new UV and infrared measurements of Reddy et al. to the existing sample compiled by Hopkins & Beacom. Then, adopting a simple model for the relation between the GRB production and the cosmic metallicity history as proposed by Langer & Norman, I show that the observed redshift distribution of the Swift GRBs can be reproduced with a fairly good accuracy. Although the results are limited by the small size of the GRB sample and the poorly understood selection biases in detection and localization of GRBs and in redshift determination, they suggest that GRBs trace both the star formation and the metallicity evolution. If the star formation history can be accurately measured with other approaches, which is presumably achievable in the near future, it will be possible to determine the cosmic metallicity evolution with the study on the redshift distribution of GRBs.Comment: 16 pages, 11 figures and 2 tables, accepted for publication in MNRAS. New version contains an updated star formation history and a review on the cosmic metallicity measuremen