La cueva de "La Roca del Frare" en la Llacuna, comarca del Penedès

La cueva de «La Roca del Frare» (citada también con el nombre de «Cova de les Rondes») está situada en las estribaciones de la Serra de Puigfred, a 50 .14' 42" de longitud Norte y 41 0 28' 15" de latitud Este (hoja 419 del mapa, 1 :50.000 del Instituto Geográfico y Catastral), a unos dos kilómetros del vecino pueblo de La Llacuna y a una altura aproximada de unos 800 metros. Se trata de una cavidad de formación tectónica enclavada en las «Roques d'en Segués». Presenta una red de galerías formadas por diaclasas abiertas, en las que hay una notable correspondencia entre las paredes opuestas. Predominan en ella los hundimientos graviclásticos sobre los quimiclásticos (figura 1). En el año 1956 un grupo de miembros colaboradores del Museo de Vilafranca del Penedes localizó una de las dos entradas de la cueva y llegaron a una sala de considerables dimensiones a la que llamaron «sala deIs cranis» por los hallazgos efectuados en ella. Depositado sobre el suelo de la cueva y sepultado en parte por un alud de piedras, hallaron el material que más adelante detallamos y una serie de huesos humanos, hoy perdidos, entre los que figuraban, al parecer, no menos de ocho cráneos.

Caracterização dos pirênios e métodos para acelerar a germinação de sementes de muruci do clone Açu

Pirênios (caroços) de murucizeiro (Byrsonima crassifolia (L.) Rich.) do clone Açu, um acesso da Coleção de Germoplasma de Fruteiras Tropicais da Embrapa Amazônia Oriental, foram caracterizados, e avaliados diferentes métodos para superação da dormência das sementes. Na caracterização dos pirênios, foram considerados os seguintes aspectos: cor, forma, peso, comprimento, diâmetro, número de sementes por pirênio e espessura das paredes internas e externas do endocarpo. Os tratamentos para superação da dormência foram: a) testemunha pirênios não-submetidos a tratamento pré-germinativo; b) imersão em água durante 24 horas; c) imersão em solução de ácido giberélico (500 mg.L-1) durante 24 horas; d) imersão em água durante 24 horas seguida de fratura no endocarpo por compressão; e) imersão em solução de ácido giberélico (500 mg.L-1) durante 24 horas seguida de fratura no endocarpo por compressão. Observou-se que os pirênios do clone Açu são ovalados, com superfície reticulada, peso de 0,62±0,09 e comprimento e diâmetro de 1,10±0,07 e 1,02±0,09 cm, respectivamente. Os pirênios geralmente contêm duas sementes (mínimo zero e máximo três), localizadas em lóculos cujas paredes externas são mais espessas que as internas. O endocarpo é permeável à água, e as sementes absorvem prontamente essa substância. As sementes representam 10,12%±2,87% do peso do pirênio. Os melhores tratamentos para sobrepujar a dormência consistiram da imersão dos pirênios em solução de ácido giberélico ou em água, seguida de fratura no endocarpo. Os resultados obtidos indicam que a germinação das sementes de muruci do clone Açu é regulada por dois mecanismos de dormência: o primeiro representado pelo espesso e córneo endocarpo, o qual é permeável à água, mas oferece resistência mecânica ao crescimento do embrião, e o segundo, devido à dormência fisiológica.

'La Manteria'. Pinturas murales de la iglesia de Santo Tomás de Villanueva

La iglesia de Santo Tomás de Villanueva de Zaragoza es lo único que se conserva de lo que fuera el convento de agustinos observantes, llamado popularmente convento de la Mantería por ubicarse en la plaza del mismo nombre. Fué edificada entre 1663 y 1683 bajo el patronazgo del arzobispo de Zaragoza don Francisco Gamboa. Es un edificio barroco construido en ladrillo, con planta de cruz latina, de una sola nave, cubierta en sus tramos y brazos por cúpulas elípticas, siendo semiesférica la del crucero. Lo más destacable del edificio es su decoración mural. En un principio las pinturas cubrían la totalidad de las paredes y bóvedas. Los avatares históricos, desamortización y posterior empleo como almacén, así como el deterioro por efecto de la humedad, han hecho que sólo hayan llegado hasta nosotros las pinturas de las cúpulas. La ejecución de la pintura se debe al pintor de cámara de Carlos II, Claudio Coello, ayudado por su discípulo Sebastián Muñoz y por una serie de pintores locales. Claudio Coello trabajó entre 1683 y 1684, prolongándose las tareas hasta 1686.

A Be-type star with a black-hole companion

Stellar-mass black holes have all been discovered through X-ray emission, which arises from the accretion of gas from their binary companions (this gas is either stripped from low-mass stars or supplied as winds from massive ones). Binary evolution models also predict the existence of black holes accreting from the equatorial envelope of rapidly spinning Be-type stars (stars of the Be type are hot blue irregular variables showing characteristic spectral emission lines of hydrogen). Of the ~80 Be X-ray binaries known in the Galaxy, however, only pulsating neutron stars have been found as companions. A black hole was formally allowed as a solution for the companion to the Be star MWC 656 (also known as HD 215227), although that was based on a single radial velocity curve of the Be star, a mistaken spectral classification and rough estimates of the inclination angle. Here we report observations of an accretion disk line mirroring the orbit of the Be star. This, together with an improved radial velocity curve of the Be star through fitting sharp Fe II profiles from the equatorial disk, and a refined Be classification (to that of a B1.5-B2 III star), reveals a black hole of 3.8 to 6.9 solar masses orbiting MWC 656, the candidate counterpart of the gamma-ray source AGL J2241+4454. The black hole is X-ray quiescent and fed by a radiatively inefficient accretion flow giving a luminosity less than 1.6 x 10-7 times the Eddington luminosity. This implies that Be binaries with black-hole companions are difficult to detect by conventional X-ray surveys.

The star forming region Monoceros R2 as a gamma-ray source

After the release of the gamma-ray source catalog produced by the Fermi satellite during its first two years of operation, a significant fraction of sources still remain unassociated at lower energies. In addition to well-known high-energy emitters (pulsars, blazars, supernova remnants, etc.), theoretical expectations predict new classes of gamma-ray sources. In particular, gamma-ray emission could be associated with some of the early phases of stellar evolution, but this interesting possibility is still poorly understood. Aims: The aim of this paper is to assess the possibility of the Fermi gamma-ray source 2FGL J0607.5-0618c being associated with the massive star forming region Monoceros R2. Methods: A multi-wavelength analysis of the Monoceros R2 region is carried out using archival data at radio, infrared, X-ray, and gamma-ray wavelengths. The resulting observational properties are used to estimate the physical parameters needed to test the different physical scenarios. Results: We confirm the 2FGL J0607.5-0618c detection with improved confidence over the Fermi two-year catalog. We find that a combined effect of the multiple young stellar objects in Monoceros R2 is a viable picture for the nature of the source.

Very-High-Energy gamma rays from a Distant Quasar: How Transparent Is the Universe?

The atmospheric Cherenkov gamma-ray telescope MAGIC, designed for a low-energy threshold, has detected very-high-energy gamma rays from a giant flare of the distant Quasi-Stellar Radio Source (in short: radio quasar) 3C 279, at a distance of more than 5 billion light-years (a redshift of 0.536). No quasar has been observed previously in very-high-energy gamma radiation, and this is also the most distant object detected emitting gamma rays above 50 gigaelectron volts. Because high-energy gamma rays may be stopped by interacting with the diffuse background light in the universe, the observations by MAGIC imply a low amount for such light, consistent with that known from galaxy counts.

The changing milliarcsecond radio morphology of the gamma-ray binary LS 5039

LS 5039 is one of the few TeV emitting X-ray binaries detected so far. The powering source of its multiwavelength emission can be accretion in a microquasar scenario or wind interaction in a young nonaccreting pulsar scenario. Aims.To present new high-resolution radio images and compare them with the expected behavior in the different scenarios. Methods.We analyze Very Long Baseline Array (VLBA) radio observations that provide morphological and astrometric information at milliarcsecond scales. Results.We detect a changing morphology between two images obtained five days apart. In both runs there is a core component with a constant flux density, and an elongated emission with a position angle (PA) that changes by 12 $\pm$ $3\degr$ between both runs. The source is nearly symmetric in the first run and asymmetric in the second one. The astrometric results are not conclusive. Conclusions.A simple and shockless microquasar scenario cannot easily explain the observed changes in morphology. An interpretation within the young nonaccreting pulsar scenario requires the inclination of the binary system to be very close to the upper limit imposed by the absence of X-ray eclipses.

Confirmation of persistent radio jets in the microquasar LS 5039

We present here new observations conducted with the EVN and MERLIN of the persistent microquasar LS 5039 discovered by Paredes et al. (2000) with the VLBA. The new observations confirm the presence of an asymmetric two-sided jet reaching up to 1000 AU on the longest jet arm. The results suggest a bending of the jets with increasing distance from the core and/or precession. The origin and location of the high-energy gamma-ray emission associated with the system is discussed and an estimate of the magnetic field at the base of the jet given. Our results suggest a well collimated radio jet. We also comment on new observing strategies to be used with satellites and forthcoming detectors, since this persistent source appears to be a rather good laboratory to explore the accretion/ejection processes taking place near compact objects.

Spectral energy distribution of the gamma-ray microquasar LS 5039

The microquasar LS 5039 has recently been detected as a source of very high energy (VHE) $\gamma$-rays. This detection, that confirms the previously proposed association of LS 5039 with the EGRET source 3EG~J1824$-$1514, makes of LS 5039 a special system with observational data covering nearly all the electromagnetic spectrum. In order to reproduce the observed spectrum of LS 5039, from radio to VHE $\gamma$-rays, we have applied a cold matter dominated jet model that takes into account accretion variability, the jet magnetic field, particle acceleration, adiabatic and radiative losses, microscopic energy conservation in the jet, and pair creation and absorption due to the external photon fields, as well as the emission from the first generation of secondaries. The radiative processes taken into account are synchrotron, relativistic Bremsstrahlung and inverse Compton (IC). The model is based on a scenario that has been characterized with recent observational results, concerning the orbital parameters, the orbital variability at X-rays and the nature of the compact object. The computed spectral energy distribution (SED) shows a good agreement with the available observational data.

Desenvolvimento dos frutos de pêssego 'Aurora' e nectarina 'Sunraycer' no sul de Santa Catarina

O desenvolvimento do fruto de pessegueiro é resultado da diferenciação e do crescimento das paredes do ovário após a fecundação. A persistência e o crescimento do fruto na planta dependem das relações exatas entre os hormônios auxina, giberelina e citocinina que condicionam o desenvolvimento dos frutos, caracterizado por uma curva dupla sigmoide, com três estádios distintos. O presente trabalho teve por objetivo conhecer o comportamento dos frutos e das sementes do pêssego Aurora e da Nectarina Sunraycer durante todo o seu ciclo de desenvolvimento. O crescimento dos frutos e das sementes durante o ciclo foi determinado semanalmente, coletando-se 30 frutos de dez diferentes plantas em ramos previamente identificados. As sementes foram separadas do fruto para a determinação do peso fresco (PF) e do peso seco (PS). O crescimento dos frutos da variedade Sunraycer dá-se de forma contínua e acelerada desde a floração até a maturação, sugerindo um curto período ou a inexistência do Estágio II de crescimento. Para a variedade Aurora, a curva de crescimento é diferenciada nos três estádios (I, II e III). O raleio dos frutos deve ser feito até o início do estádio II, para a variedade Aurora e Sunraycer. As sementes das variedades Aurora e Sunraycer atingem seu tamanho máximo no estágio I de crescimento do fruto. O aumento de peso seco na semente, para a variedade Sunraycer, é praticamente inexistente no estádio III, enquanto para a variedade Aurora ocorre o maior aumento de peso seco que vai até a maturação do fruto.

Genome sequence of the Drosophila melanogaster male-killing Spiroplasma strain MSRO endosymbiont.

Spiroplasmas are helical and motile members of a cell wall-less eubacterial group called Mollicutes. Although all spiroplasmas are associated with arthropods, they exhibit great diversity with respect to both their modes of transmission and their effects on their hosts; ranging from horizontally transmitted pathogens and commensals to endosymbionts that are transmitted transovarially (i.e., from mother to offspring). Here we provide the first genome sequence, along with proteomic validation, of an endosymbiotic inherited Spiroplasma bacterium, the Spiroplasma poulsonii MSRO strain harbored by Drosophila melanogaster. Comparison of the genome content of S. poulsonii with that of horizontally transmitted spiroplasmas indicates that S. poulsonii has lost many metabolic pathways and transporters, demonstrating a high level of interdependence with its insect host. Consistent with genome analysis, experimental studies showed that S. poulsonii metabolizes glucose but not trehalose. Notably, trehalose is more abundant than glucose in Drosophila hemolymph, and the inability to metabolize trehalose may prevent S. poulsonii from overproliferating. Our study identifies putative virulence genes, notably, those for a chitinase, the H2O2-producing glycerol-3-phosphate oxidase, and enzymes involved in the synthesis of the eukaryote-toxic lipid cardiolipin. S. poulsonii also expresses on the cell membrane one functional adhesion-related protein and two divergent spiralin proteins that have been implicated in insect cell invasion in other spiroplasmas. These lipoproteins may be involved in the colonization of the Drosophila germ line, ensuring S. poulsonii vertical transmission. The S. poulsonii genome is a valuable resource to explore the mechanisms of male killing and symbiont-mediated protection, two cardinal features of many facultative endosymbionts. IMPORTANCE: Most insect species, including important disease vectors and crop pests, harbor vertically transmitted endosymbiotic bacteria. These endosymbionts play key roles in their hosts' fitness, including protecting them against natural enemies and manipulating their reproduction in ways that increase the frequency of symbiont infection. Little is known about the molecular mechanisms that underlie these processes. Here, we provide the first genome draft of a vertically transmitted male-killing Spiroplasma bacterium, the S. poulsonii MSRO strain harbored by D. melanogaster. Analysis of the S. poulsonii genome was complemented by proteomics and ex vivo metabolic experiments. Our results indicate that S. poulsonii has reduced metabolic capabilities and expresses divergent membrane lipoproteins and potential virulence factors that likely participate in Spiroplasma-host interactions. This work fills a gap in our knowledge of insect endosymbionts and provides tools with which to decipher the interaction between Spiroplasma bacteria and their well-characterized host D. melanogaster, which is emerging as a model of endosymbiosis.

Observation of VHE γ-rays from Cassiopeia A with the MAGIC telescope

Aims:We searched for very high energy (VHE) γ-ray emission from the supernova remnant Cassiopeia A Methods: The shell-type supernova remnant Cassiopeia A was observed with the 17 m MAGIC telescope between July 2006 and January 2007 for a total time of 47 h. Results: The source was detected above an energy of 250 GeV with a significance of 5.2σ and a photon flux above 1 TeV of (7.3 ± 0.7_stat ± 2.2_sys) × 10-13 cm-2s-1. The photon spectrum is compatible with a power law dN/dE ∝ E-Γ with a photon index Γ = 2.3 ± 0.2_stat ± 0.2_sys. The source is point-like within the angular resolution of the telescope.

Gamma-ray emission from microquasars: a numerical model for LSI+61º303

We explore the possible association between the microquasar LSI +61°303 and the EGRET source 2CG 135+01/3EG J0241+6103 by studying, with a detailed numerical model, whether this system can produce the emission and the variability detected by EGRET (>100 MeV) through inverse Compton (IC) scattering. Our numerical approach considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet, interacting with both the radiation and the magnetic fields, taking into account the Thomson and Klein-Nishina regimes of interaction. Our results reproduce the observed spectral characteristics and variability at γ-rays, thus strengthening the identification of LSI +61°303 as a high-energy γ-ray source.

Long-term X-ray variability of the microquasar system LS5039/RX J1826.2-1450

We report on the results of the spectral and timing analysis of a BeppoSAX observation of the microquasar system LS 5039/RX J1826.2-1450. The source was found in a low-flux state with Fx(1-10 keV)= 4.7 x 10^{-12} erg cm^{-2} s^{-1}, which represents almost one order of magnitude lower than a previous RXTE observation 2.5 years before. The 0.1--10 keV spectrum is described by an absorbed power-law continuum with photon-number spectral index Gamma=1.8+-0.2 and hydrogen column density of NH=1.0^{+0.4}_{-0.3} x 10^{22} cm^{-2}. According to the orbital parameters of the system the BeppoSAX observation covers the time of an X-ray eclipse should one occur. However, the 1.6-10 keV light curve does not show evidence for such an event, which allows us to give an upper limit to the inclination of the system. The low X-ray flux detected during this observation is interpreted as a decrease in the mass accretion rate onto the compact object due to a decrease in the mass-loss rate from the primary.

Deep radio images of the HEGRA and Whipple TeV sources in the Cygnus OB2 region.

The modern generation of Cherenkov telescopes has revealed a new population of gamma-ray sources in the Galaxy. Some of them have been identified with previously known X-ray binary systems while other remain without clear counterparts a lower energies. Our initial goal here was reporting on extensive radio observations of the first extended and yet unidentified source, namely TeV J2032+4130. This object was originally detected by the HEGRA telescope in the direction of the Cygnus OB2 region and its nature has been a matter of debate during the latest years. The situation has become more complex with the Whipple and MILAGRO telescopes new TeV detections in the same field which could be consistent with the historic HEGRA source, although a different origin cannot be ruled out. Aims.We aim to pursue our radio exploration of the TeV J2032+4130 position that we initiated in a previous paper but taking now into account the latest results from new Whipple and MILAGRO TeV telescopes. The data presented here are an extended follow up of our previous work. Methods.Our investigation is mostly based on interferometric radio observations with the Giant Metre Wave Radio Telescope (GMRT) close to Pune (India) and the Very Large Array (VLA) in New Mexico (USA). We also conducted near infrared observations with the 3.5 m telescope and the OMEGA2000 camera at the Centro Astronómico Hispano Alemán (CAHA) in Almería (Spain). Results.We present deep radio maps centered on the TeV J2032+4130 position at different wavelengths. In particular, our 49 and 20 cm maps cover a field of view larger than half a degree that fully includes the Whipple position and the peak of MILAGRO emission. Our most important result here is a catalogue of 153 radio sources detected at 49 cm within the GMRT antennae primary beam with a full width half maximum (FWHM) of 43 arc-minute. Among them, peculiar sources inside the Whipple error ellipse are discussed in detail, including a likely double-double radio galaxy and a one-sided jet source of possible blazar nature. This last object adds another alternative counterpart possibility to be considered for both the HEGRA, Whipple and MILAGRO emission. Moreover, our multi-configuration VLA images reveal the non-thermal extended emission previously reported by us with improved angular resolution. Its non-thermal spectral index is also confirmed thanks to matching beam observations at the 20 and 6 cm wavelengths.