Evolutionary reconstruction of a hairpin deleted from the genome of an RNA virus.

The intercistronic region between the maturation and coat-protein genes of RNA phage MS2 contains important regulatory and structural information. The sequence participates in two adjacent stem-loop structures, one of which, the coat-initiator hairpin, controls coat-gene translation and is thus under strong selection pressure. We have removed 19 out of the 23 nucleotides constituting the intercistronic region, thereby destroying the capacity of the phage to build the two hairpins. The deletion lowered coat-protein yield more than 1000-fold, and the titer of the infectious clone carrying the deletion dropped 10 orders of magnitude as compared with the wild type. Two types of revertants were recovered. One had, in two steps, recruited 18 new nucleotides that served to rebuild the two hairpins and the lost Shine-Dalgarno sequence. The other type had deleted an additional six nucleotides, which allowed the reconstruction of the Shine-Dalgarno sequence and the initiator hairpin, albeit by sacrificing the remnants of the other stem-loop. The results visualize the immense genetic repertoire created by, what appears as, random RNA recombination. It would seem that in this genetic ensemble every possible new RNA combination is represented.

The nuclear region of the spiral galaxy M81.

Very-long-baseline radio interferometry images of the nuclear region of the nearby spiral galaxy M81 reveal the most compact galactic core outside the Galaxy of which the size has been determined: 700 x 300 astronomical units (AU). The observations exclude a starburst or supernova interpretation for the core. Instead they favor an active galactic nucleus. There is evidence for a northeastern jet bent by approximately 35 degrees over a length scale from 700 to 4000 AU. The jet is, on average, directed toward an extended emission region, probably a radio lobe, about 1 kiloparsec (kpc) away from the core. A corresponding emission region was found in the southwest at a distance of only 30 pc from the core. The observed jet is extremely stable and likely to be associated with a steady-state channel. There is no detectable motion along the jet beyond the nominal value of -60 +/- 60 km.s-1. The level of activities in the core region of M81 is intermediate between that of SgrA* and that of powerful radio galaxies and quasars.

Evidence against the exon theory of genes derived from the triose-phosphate isomerase gene.

The exon theory of genes proposes that the introns of protein-encoding nuclear genes are remnants of the DNA spacers between ancient minigenes. The discovery of an intron at a predicted position in the triose-phosphate isomerase (EC 5.3.1.1) gene of Culex mosquitoes has been hailed as an evidential pillar of the theory. We have found that that intron is also present in Aedes mosquitoes, which are closely related to Culex, but not in the phylogenetically more distant Anopheles, nor in the fly Calliphora vicina, nor in the moth Spodoptera littoralis. The presence of this intron in Culex and Aedes is parsimoniously explained as the result of an insertion in a recent common ancestor of these two species rather than as the remnant of an ancient intron. The absence of the intron in 19 species of very diverse organisms requires at least 10 independent evolutionary losses in order to be consistent with the exon theory.

Functional expression of low density lipoprotein receptor-related protein is controlled by receptor-associated protein in vivo.

The 39-kDa receptor-associated protein (RAP) associates with the multifunctional low density lipoprotein (LDL) receptor-related protein (LRP) and thereby prevents the binding of all known ligands, including alpha 2-macroglobulin and chylomicron remnants. RAP is predominantly localized in the endoplasmic reticulum, raising the possibility that it functions as a chaperone or escort protein in the biosynthesis or intracellular transport of LRP. Here we have used gene targeting to show that RAP promotes the expression of functional LRP in vivo. The amount of mature, processed LRP is reduced in liver and brain of RAP-deficient mice. As a result, hepatic clearance of alpha 2-macroglobulin is impaired and remnant lipoproteins accumulate in the plasma of RAP-deficient mice that also lack functional LDL receptors. These results are consistent with the hypothesis that RAP stabilizes LRP within the secretory pathway. They also suggest a further mechanism by which the activity of an endocytic receptor may be modulated in vivo.

Obesidade e genes candidatos: estudo de associação em populações quilombolas do Vale do Ribeira-SP

A obesidade comum é atualmente um dos problemas de saúde pública mais importante no mundo, frequentemente associada a outros distúrbios tais como hipertensão, diabetes, doenças cardiovasculares e câncer. Apesar da alta prevalência de obesidade em diversas populações, muitos dos estudos relacionados aos seus fatores de risco genéticos foram realizados com indivíduos de ascendência europeia ou asiática, mas foram poucos os realizados com populações de origem africana ou nativas americanas. Nosso trabalho tem por objetivo geral investigar potenciais fatores de risco genéticos associados ao sobrepeso e à obesidade em populações afrodescendentes remanescentes de quilombos do Vale do Ribeira - SP, comunidades rurais semi-isoladas, previamente bem caracterizadas do ponto de vista clínico, genealógico e genético-populacional. Nossa amostra constituiu-se de 759 indivíduos, pertencentes a doze populações de remanescentes de quilombos (Abobral, São Pedro, Galvão, Ivaporunduva, Pedro Cubas, André Lopes, Nhunguara, Sapatu, Pilões, Maria Rosa, Poça e Reginaldo), dos quais foram obtidos amostras de DNA, dados clínicos, informações genealógicas e medidas antropométricas. A investigação dos fatores de risco genéticos associados ao sobrepeso/obesidade foi realizada por duas abordagens: (1) estudo de associação baseado em famílias (N = 584, 59 famílias) e (2) estudo de associação populacional com indivíduos não aparentados (N=305). Foram selecionados para estudo nove polimorfismos em oito genes candidatos: LEP rs2167270, LEPR rs1137101, ADRB2 rs1042713, PPARG rs1801282, PLIN1 rs2289487, RETN rs1862513, INSIG2 rs7566605, FTO rs1121980 e FTO rs1421085. As análises de associação baseadas em família indicaram que, nessas populações, apenas o polimorfismo PLIN1 rs2289487 está associado significativamente com o grupo de risco em relação à razão cintura-quadril (RCQ >=0,85 para mulheres e >=0,90 para homens; P=0,013). Aparentemente não existem trabalhos anteriores que verificaram a associação deste polimorfismo com a obesidade por essa metodologia. As análises do estudo populacional com indivíduos não aparentados mostraram associação significativa entre: (i) o alelo G no polimorfismo LEPR rs1137101 e a variação do índice de massa corporal (IMC; P=0,027); (ii) o alelo G do polimorfismo LEPR rs1137101 e o fenótipo de sobrepeso/obesidade (IMC>=25 Kg/m²; P=0,027); (iii) o alelo G no polimorfismo ADRB2 rs1042713 e o fenótipo de risco (IMC>=25 Kg/m²; P=0,029); (iv) o polimorfismo PLIN1 rs2289487 (genótipo GG) e os menores valores do IMC (P=0,025); (v) o polimorfismo FTO rs1121980 (alelo G) e o fenótipo de risco (IMC>=25 Kg/m²), assim como a variação do IMC (P=0,037 e P=0,022 respectivamente); e (vi) o alelo A no polimorfismo FTO rs1421085 e maiores valores da circunferência da cintura (Cc; P=0,016) e da razão cintura-quadril (RCQ; P=0,030). Tomados em conjunto, nossos resultados sugerem a participação dos genes LEP, LEPR, ADRB2, PLIN1 e FTO no aumento da predisposição ao sobrepeso e à obesidade nas populações remanescentes de quilombos. Por fim, as elevadas estimativas de herdabilidade dos três fenótipos investigados (IMC=33%, Cc=33% e RCQ=70%) reforçam a relevância do papel dos fatores genéticos no acúmulo de gordura corporal. O trabalho apresentado é resultado de uma investigação cuidadosa sobre os componentes genéticos associados à regulação do peso corporal em uma população brasileira afrodescendente (com características históricas, ambientais e genéticas peculiares), corroborando a hipótese de que a obesidade comum nas populações quilombolas do Vale do Ribeira é condicionada por um mecanismo poligênico modulado por fatores ambientais importantes como o sedentarismo e a transição nutricional

The ionized gas in the CALIFA early-type galaxies I. Mapping two representative cases: NGC 6762 and NGC 5966

As part of the ongoing CALIFA survey, we have conducted a thorough bidimensional analysis of the ionized gas in two E/S0 galaxies, NGC 6762 and NGC 5966, aiming to shed light on the nature of their warm ionized ISM. Specifically, we present optical (3745–7300 Å) integral field spectroscopy obtained with the PMAS/PPAK integral field spectrophotometer. Its wide field-of-view (1′ × 1′) covers the entire optical extent of each galaxy down to faint continuum surface brightnesses. To recover the nebular lines, we modeled and subtracted the underlying stellar continuum from the observed spectra using the STARLIGHT spectral synthesis code. The pure emission-line spectra were used to investigate the gas properties and determine the possible sources of ionization. We show the advantages of IFU data in interpreting the complex nature of the ionized gas in NGC 6762 and NGC 5966. In NGC 6762, the ionized gas and stellar emission display similar morphologies, while the emission line morphology is elongated in NGC 5966, spanning ~6 kpc, and is oriented roughly orthogonal to the major axis of the stellar continuum ellipsoid. Whereas gas and stars are kinematically aligned in NGC 6762, the gas is kinematically decoupled from the stars in NGC 5966. A decoupled rotating disk or an “ionization cone” are two possible interpretations of the elongated ionized gas structure in NGC 5966. The latter would be the first “ionization cone” of such a dimension detected within a weak emission-line galaxy. Both galaxies have weak emission-lines relative to the continuum[EW(Hα) ≲ 3 Å] and have very low excitation, log([OIII]λ5007/Hβ) ≲ 0.5. Based on optical diagnostic ratios ([OIII]λ5007/Hβ, [NII]λ6584/Hα, [SII]λ6717, 6731/Hα, [OI]λ6300/Hα), both objects contain a LINER nucleus and an extended LINER-like gas emission. The emission line ratios do not vary significantly with radius or aperture, which indicates that the nebular properties are spatially homogeneous. The gas emission in NGC 6762 can be best explained by photoionization by pAGB stars without the need of invoking any other excitation mechanism. In the case of NGC 5966, the presence of a nuclear ionizing source seems to be required to shape the elongated gas emission feature in the “ionization cone” scenario, although ionization by pAGB stars cannot be ruled out. Further study of this object is needed to clarify the nature of its elongated gas structure.

No surviving evolved companions of the progenitor of SN 1006

Type Ia supernovae are thought to occur when a white dwarf made of carbon and oxygen accretes sufficient mass to trigger a thermonuclear explosion(1). The accretion could be slow, from an unevolved (main-sequence) or evolved (subgiant or giant) star(2,3) (the single-degenerate channel), or rapid, as the primary star breaks up a smaller orbiting white dwarf(3,4) (the double-degenerate channel). A companion star will survive the explosion only in the single-degenerate channel(5). Both channels might contribute to the production of type Ia supernovae(6,7), but the relative proportions of their contributions remain a fundamental puzzle in astronomy. Previous searches for remnant companions have revealed one possible case for SN 1572 (refs 8, 9), although that has been questioned(10). More recently, observations have restricted surviving companions to be small, main-sequence stars(11-13), ruling out giant companions but still allowing the single-degenerate channel. Here we report the results of a search for surviving companions of the progenitor of SN 1006 (ref. 14). None of the stars within 4 arc minutes of the apparent site of the explosion is associated with the supernova remnant, and we can firmly exclude all giant and subgiant stars from being companions of the progenitor. In combination with previous results, our findings indicate that fewer than 20 per cent of type Ia supernovae occur through the single-degenerate channel.

Georges de La Tour : the Status of Scholarship

Seventeenth-century French painter, Georges de La Tour, was a forgotten artist. His rediscovery in the nineteenth century set off a firestorm of research and a hunt to find more works by the artist. One problem after another arose as scholars attempted to define the artist by his works, his style, and the remnants of his personal history. There remains a volume of contradictory reports, authentication issues, and new scientific techniques which continue to influence study on the artist.

Infrared identification of 2XMM J191043.4+091629.4

Context. We report the infrared identification of the X-ray source 2XMM J191043.4+091629.4, which was detected by XMM-Newton/EPIC in the vicinity of the Galactic supernova remnant W49B. Aims. The aim of this work is to establish the nature of the X-ray source 2XMM J191043.4+091629.4 studying both the infrared photometry and spectroscopy of the companion. Methods. We analysed UKIDSS images around the best position of the X-ray source and obtained spectra of the best candidate using NICS in the Telescopio Nazionale Galileo (TNG) 3.5-m telescope. We present photometric and spectroscopic TNG analyses of the infrared counterpart of the X-ray source, identifying emission lines in the K-band. The H-band spectra does not present any significant feature. Results. We have shown that the Brackett γ H i at 2.165 μm, and He i at 2.184 μm and at 2.058 μm are significantly present in the infrared spectrum. The CO bands are also absent from our spectrum. Based on these results and the X-ray characteristics of the source, we conclude that the infrared counterpart is an early B-type supergiant star with an E(B − V) = 7.6 ± 0.3 at a distance of 16.0 ± 0.5 kpc. This would be, therefore, the first high-mass X-ray binary in the Outer Arm at galactic longitudes of between 30° and 60°.

Pulsar timing irregularities and the imprint of magnetic field evolution

Context. The rotational evolution of isolated neutron stars is dominated by the magnetic field anchored to the solid crust of the star. Assuming that the core field evolves on much longer timescales, the crustal field evolves mainly though Ohmic dissipation and the Hall drift, and it may be subject to relatively rapid changes with remarkable effects on the observed timing properties. Aims. We investigate whether changes of the magnetic field structure and strength during the star evolution may have observable consequences in the braking index n. This is the most sensitive quantity to reflect small variations of the timing properties that are caused by magnetic field rearrangements. Methods. We performed axisymmetric, long-term simulations of the magneto-thermal evolution of neutron stars with state-of-the-art microphysical inputs to calculate the evolution of the braking index. Relatively rapid magnetic field modifications can be expected only in the crust of neutron stars, where we focus our study. Results. We find that the effect of the magnetic field evolution on the braking index can be divided into three qualitatively different stages depending on the age and the internal temperature: a first stage that may be different for standard pulsars (with n ~ 3) or low field neutron stars that accreted fallback matter during the supernova explosion (systematically n < 3); in a second stage, the evolution is governed by almost pure Ohmic field decay, and a braking index n > 3 is expected; in the third stage, at late times, when the interior temperature has dropped to very low values, Hall oscillatory modes in the neutron star crust result in braking indices of a high absolute value and both positive and negative signs. Conclusions. Current magneto-thermal evolution models predict a large contribution to the timing noise and, in particular, to the braking index, from temporal variations of the magnetic field. Models with strong (≳ 1014 G) multipolar or toroidal components, even with a weak (~1012 G) dipolar field are consistent with the observed trend of the timing properties.

Nuevos materiales absorbentes acústicos obtenidos a partir de restos de botellas de plástico

En el ámbito de acústica de la edificación es común el uso de materiales fibrosos como materiales absorbentes acústicos. Uno de estos materiales cada vez más utilizado es la lana de poliéster. Un problema que presenta el chip virgen de poliéster es que se obtiene del petróleo, cuyo precio no hace más que incrementarse en los últimos años. En este trabajo se presenta una lana de poliéster alternativa, obtenida mediante el tratamiento del PET, a través del conveniente ciclo de reciclado de botellas de plástico. Se comparan valores del coeficiente de absorción; en incidencia normal y en cámara reverberante de los materiales elaborados a partir de chip virgen y de las nuevas lanas obtenidas del PET. Además, se propone un modelo empírico de comportamiento acústico de estas nuevas lanas. Los resultados obtenidos han sido favorables, la fibra virgen ya ha sido sustituida por fibra reciclada en su proceso de fabricación.

Una nueva rábita en la playa de Guardamar del Segura: la rábita de El Moncayo

Se publican las noticias que ha arrojado la excavación en 2004 de unos muros situados en la denominada playa de El Moncayo. Los hallazgos se sitúan a unos 3 kilómetros al Sur del casco urbano de Guardamar del Segura; a unos 135 m. en dirección Norte está la Torre del Descargador (torre almenara de los siglos IV/X y V/XI), a unos 3,5 kilómetros se localiza El Castillo de Guardamar (de los siglos VIII a.C. al XIX) y, un poco más al Norte, a unos 4 kilómetros, en las proximidades de la desembocadura del Segura, los oratorios o rábitas de las dunas de Guardamar. Se dan a conocer los restos arquitectónicos y cerámicos aparecidos en la excavación del 2004 que se interpretan como de restos del recinto de una rábita o mezquitilla (cuando se excave más se verá si está aislada o hay más edificios similares), se presentan unos apuntes al hilo de la orientación de la rábita de El Moncayo y un estudio de la moneda andalusí hallada en la excavación de El Moncayo (datables entre en 429/1037-8 y 433/1041-2).

IRAS 18357-0604 – an analogue of the galactic yellow hypergiant IRC +10420?

Context. Yellow hypergiants represent a short-lived evolutionary episode experienced by massive stars as they transit to and from a red supergiant phase. As such, their properties provide a critical test of stellar evolutionary theory, while recent observations unexpectedly suggest that a subset may explode as Type II supernovae. Aims. The galactic yellow hypergiant IRC +10420 is a cornerstone system for understanding this phase since it is the strongest post-RSG candidate known, has demonstrated real-time evolution across the Hertzsprung-Russell diagram and been subject to extensive mass loss. In this paper we report on the discovery of a twin of IRC +10420 - IRAS 18357-0604. Methods. Optical and near-IR spectroscopy are used to investigate the physical properties of IRAS 18357-0604 and also provide an estimate of its systemic velocity, while near- to mid-IR photometry probes the nature of its circumstellar environment. Results. These observations reveal pronounced spectral similarities between IRAS 18357-0604 and IRC +10420, suggesting comparable temperatures and wind geometries. IR photometric data reveals a similarly dusty circumstellar environment, although historical mass loss appears to have been heavier in IRC +10420. The systemic velocity implies a distance compatible with the red supergiant-dominated complex at the base of the Scutum Crux arm; the resultant luminosity determination is consistent with a physical association but suggests a lower initial mass than inferred for IRC +10420 (≲20 M⊙ versus ~40 M⊙). Evolutionary predictions for the physical properties of supernova progenitors derived from ~18–20 M⊙ stars – or ~12–15 M⊙ stars that have experienced enhanced mass loss as red supergiants – compare favourably with those of IRAS 18357-0604, which in turn appears to be similar to the the progenitor of SN2011dh; it may therefore provide an important insight into the nature of the apparently H-depleted yellow hypergiant progenitors of some Type IIb SNe.

The little-studied cluster Berkeley 90 I. LS III +46 11: a very massive O3.5 If* + O3.5 If* binary

Context. It appears that most (if not all) massive stars are born in multiple systems. At the same time, the most massive binaries are hard to find owing to their low numbers throughout the Galaxy and the implied large distances and extinctions. Aims. We want to study LS III +46 11, identified in this paper as a very massive binary; another nearby massive system, LS III +46 12; and the surrounding stellar cluster, Berkeley 90. Methods. Most of the data used in this paper are multi-epoch high S/N optical spectra, although we also use Lucky Imaging and archival photometry. The spectra are reduced with dedicated pipelines and processed with our own software, such as a spectroscopic-orbit code, CHORIZOS, and MGB. Results. LS III +46 11 is identified as a new very early O-type spectroscopic binary [O3.5 If* + O3.5 If*] and LS III +46 12 as another early O-type system [O4.5 V((f))]. We measure a 97.2-day period for LS III +46 11 and derive minimum masses of 38.80 ± 0.83 M⊙ and 35.60 ± 0.77 M⊙ for its two stars. We measure the extinction to both stars, estimate the distance, search for optical companions, and study the surrounding cluster. In doing so, a variable extinction is found as well as discrepant results for the distance. We discuss possible explanations and suggest that LS III +46 12 may be a hidden binary system where the companion is currently undetected.

On the formation and evolution of the first Be star in a black hole binary MWC 656

We find that the formation of MWC 656 (the first Be binary containing a black hole) involves a common envelope phase and a supernova explosion. This result supports the idea that a rapidly rotating Be star can emerge out of a common envelope phase, which is very intriguing because this evolutionary stage is thought to be too fast to lead to significant accretion and spin up of the B star. We predict ∼10–100 of B-BH binaries to currently reside in the Galactic disc, among which around 1/3 contain a Be star, but there is only a small chance to observe a system with parameters resembling MWC 656. If MWC 656 is representative of intrinsic Galactic Be-BH binary population, it may indicate that standard evolutionary theory needs to be revised. This would pose another evolutionary problem in understanding black hole (BH) binaries, with BH X-ray novae formation issue being the prime example. Future evolution of MWC 656 with an ∼5 M⊙ BH and with an ∼13 M⊙ main-sequence companion on an ∼60 d orbit may lead to the formation of a coalescing BH–NS (neutron star) system. The estimated Advanced LIGO/Virgo detection rate of such systems is up to ∼0.2 yr−1. This empirical estimate is a lower limit as it is obtained with only one particular evolutionary scenario, the MWC 656 binary. This is only a third such estimate available (after Cyg X-1 and Cyg X-3), and it lends additional support to the existence of so far undetected BH–NS binaries.