Radio detections towards unidentified variable EGRET sources

A considerable fraction of the -ray sources discovered with the Energetic Gamma-Ray Experiment Telescope (EGRET) remain unidentified. The EGRET sources that have been properly identified are either pulsars or variable sources at both radio and gamma-ray wavelengths. Most of the variable sources are strong radio blazars. However, some low galactic-latitude EGRET sources, with highly variable -ray emission, lack any evident counterpart according to the radio data available until now. Aims. The primary goal of this paper is to identify and characterise the potential radio counterparts of four highly variable -ray sources in the galactic plane through mapping the radio surroundings of the EGRET confidence contours and determining the variable radio sources in the field whenever possible. Methods. We have carried out a radio exploration of the fields of the selected EGRET sources using the Giant Metrewave Radio Telescope (GMRT) interferometer at 21 cm wavelength, with pointings being separated by months. Results. We detected a total of 151 radio sources. Among them, we identified a few radio sources whose flux density has apparently changed on timescales of months. Despite the limitations of our search, their possible variability makes these objects a top-priority target for multiwavelength studies of the potential counterparts of highly variable, unidentified gamma-ray sources.

Faint arc-minute extended radio emission around Cygnus X-3

Aims.We revisit the vicinity of the microquasar Cygnus X-3 at radio wavelengths. We aim to improve our previous search for possible associated extended radio features/hot spots in the position angle of the Cygnus X-3 relativistic jets focusing on shorter angular scales than previously explored. Methods.Our work is mostly based on analyzing modern survey and archive radio data, mainly including observations carried out with the Very Large Array and the Ryle Telescopes. We also used deep near-infrared images that we obtained in 2005. Results.We present new radio maps of the Cygnus X-3 field computed after combining multi-configuration Very Large Array archive data at 6 cm and different observing runs at 2 cm with the Ryle Telescope. These are probably among the deepest radio images of Cygnus X-3 reported to date at cm wavelengths. Both interferometers reveal an extended radio feature within a few arc-minutes of the microquasar position, thus making our detection more credible. Moreover, this extended emission is possibly non-thermal, although this point still needs confirmation. Its physical connection with the microquasar is tentatively considered under different physical scenarios. We also report on the serendipitous discovery of a likely Fanaroff-Riley type II radio galaxy only away from Cygnus X-3.

Leptonic secondary emission in a hadronic microquasar model

Context.It has been proposed that the origin of the very high-energy photons emitted from high-mass X-ray binaries with jet-like features, so-called microquasars (MQs), is related to hadronic interactions between relativistic protons in the jet and cold protons of the stellar wind. Leptonic secondary emission should be calculated in a complete hadronic model that includes the effects of pairs from charged pion decays inside the jets and the emission from pairs generated by gamma-ray absorption in the photosphere of the system. Aims.We aim at predicting the broadband spectrum from a general hadronic microquasar model, taking into account the emission from secondaries created by charged pion decay inside the jet. Methods.The particle energy distribution for secondary leptons injected along the jets is consistently derived taking the energy losses into account. The spectral energy distribution resulting from these leptons is calculated after assuming different values of the magnetic field inside the jets. We also compute the spectrum of the gamma-rays produced by neutral pion-decay and processed by electromagnetic cascades under the stellar photon field. Results.We show that the secondary emission can dominate the spectral energy distribution at low energies (~1 MeV). At high energies, the production spectrum can be significantly distorted by the effect of electromagnetic cascades. These effects are phase-dependent, and some variability modulated by the orbital period is predicted.

Exploring the connection between the stellar wind and the non-thermal emission in LS 5039

Context.LS 5039 has been observed with several X-ray instruments so far showing quite steady emission in the long term and no signatures of accretion disk. The source also presents X-ray variability at orbital timescales in flux and photon index. The system harbors an O-type main sequence star with moderate mass-loss. At present, the link between the X-rays and the stellar wind is unclear. Aims.We study the X-ray fluxes, spectra, and absorption properties of LS 5039 at apastron and periastron passages during an epoch of enhanced stellar mass-loss, and the long term evolution of the latter in connection with the X-ray fluxes. Methods.New XMM-Newton observations were performed around periastron and apastron passages in September 2005, when the stellar wind activity was apparently higher. April 2005 Chandra observations on LS 5039 were revisited. Moreover, a compilation of H EW data obtained since 1992, from which the stellar mass-loss evolution can be approximately inferred, was carried out. Results.XMM-Newton observations show higher and harder emission around apastron than around periastron. No signatures of thermal emission or a reflection iron line indicating the presence of an accretion disk are found in the spectrum, and the hydrogen column density () is compatible with being the same in both observations and consistent with the interstellar value. 2005 Chandra observations show a hard X-ray spectrum, and possibly high fluxes, although pileup effects preclude conclusive results from being obtained. The H EW shows yearly variations of 10%, and does not seem to be correlated with X-ray fluxes obtained at similar phases, unlike what is expected in the wind accretion scenario. Conclusions.2005 XMM-Newton and Chandra observations are consistent with 2003 RXTE/PCA results, namely moderate flux and spectral variability at different orbital phases. The constancy of the seems to imply that either the X-ray emitter is located at 1012 cm from the compact object, or the density in the system is 3 to 27 times smaller than that predicted by a spherical symmetric wind model. We suggest that the multiwavelength non-thermal emission of LS 5039 is related to the observed extended radio jets and is unlikely to be produced inside the binary system.

Variable Very-High-Energy Gamma-Ray Emission from the Microquasar LS I +61 303

Microquasars are binary star systems with relativistic radio-emitting jets. They are potential sources of cosmic rays and can be used to elucidate the physics of relativistic jets. We report the detection of variable gamma-ray emission above 100 gigaelectron volts from the microquasar LS I 61 + 303. Six orbital cycles were recorded. Several detections occur at a similar orbital phase, which suggests that the emission is periodic. The strongest gamma-ray emission is not observed when the two stars are closest to one another, implying a strong orbital modulation of the emission or absorption processes.

INTEGRAL and XMM-Newton observations towards the unidentified MeV source GRO J1411-64.

The COMPTEL unidentified source GRO J1411-64 was observed by INTEGRAL, and its central part, also by XMM-Newton. The data analysis shows no hint for new detections at hard X-rays. The upper limits in flux herein presented constrain the energy spectrum of whatever was producing GRO J1411-64, imposing, in the framework of earlier COMPTEL observations, the existence of a peak in power output located somewhere between 300-700 keV for the so-called low state. The Circinus Galaxy is the only source detected within the 4$\sigma$ location error of GRO J1411-64, but can be safely excluded as the possible counterpart: the extrapolation of the energy spectrum is well below the one for GRO J1411-64 at MeV energies. 22 significant sources (likelihood $> 10$) were extracted and analyzed from XMM-Newton data. Only one of these sources, XMMU J141255.6-635932, is spectrally compatible with GRO J1411-64 although the fact the soft X-ray observations do not cover the full extent of the COMPTEL source position uncertainty make an association hard to quantify and thus risky. The unique peak of the power output at high energies (hard X-rays and gamma-rays) resembles that found in the SED seen in blazars or microquasars. However, an analysis using a microquasar model consisting on a magnetized conical jet filled with relativistic electrons which radiate through synchrotron and inverse Compton scattering with star, disk, corona and synchrotron photons shows that it is hard to comply with all observational constrains. This and the non-detection at hard X-rays introduce an a-posteriori question mark upon the physical reality of this source, which is discussed in some detail.

Possible hot spots excited by the relativistic jets of Cygnus X-3

We present the results of a deep search for associated radio features in the vicinity of the microquasar Cygnus X-3. The motivation behind is to find out evidence for interaction between its relativistic jets and the surrounding interstellar medium, which could eventually allow us to perform calorimetry of the total energy released by this microquasar during its flaring lifetime. Remarkably, two radio sources with mJy emission level at centimeter wavelengths have been detected in excellent alignment with the position angle of the inner radio jets. We propose that these objects could be the hot spots where the relativitic outflow collides with the ambient gas in analogy with Fanaroff-Riley II radio galaxies. These candidate hot spots are within a few arc-minutes of Cygnus X-3 and, if physically related, the full linear extent of the jet would reach tens of parsecs. We discuss here the evidence currently available to support this hypothesis based on both archival data and our own observations.

Informe de resultats de la recerca: "Avaluació dels continguts especí­fics de la formació del mestre d'educació musical de la Universitat de Barcelona: punts forts i punts febles"

Aquest informe és un resum dels resultats obtinguts pel grup de recerca GREMI de la UB. Aquests resultats mostren el perfil de l'alumnat i del professorat tutor del pràcticum II de la titulació de Mestre en Educació Musical a la UB i les seves opinions respecte als continguts musicals treballats durant aquests estudis i llur aplicabilitat a l'escola primària

Qüestionari d'egresats de mestre en Educació Musical 2005-08

És un qüestionari d'una recerca sobre egresats d'Educació Musical a la UB

An AdS/QCD model from tachyon condensation: II

A simple holographic model is presented and analyzed that describes chiral symmetry breaking and the physics of the meson sector in QCD. This is a bottom-up model that incorporates string theory ingredients like tachyon condensation which is expected to be the main manifestation of chiral symmetry breaking in the holographic context. As a model for glue the Kuperstein-Sonnenschein background is used. The structure of the flavor vacuum is analyzed in the quenched approximation. Chiral symmetry breaking is shown at zero temperature. Above the deconfinement transition chiral symmetry is restored. A complete holographic renormalization is performed and the chiral condensate is calculated for different quark masses both at zero and non-zero temperatures. The 0++, 0¿+, 1++, 1¿¿ meson trajectories are analyzed and their masses and decay constants are computed. The asymptotic trajectories are linear. The model has one phenomenological parameter beyond those of QCD that affects the 1++, 0¿+ sectors. Fitting this parameter we obtain very good agreement with data. The model improves in several ways the popular hard-wall and soft wall bottom-up models.

La cueva de la Roca del Frare en la Llacuna

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.

Hallazgos en Tarragona

Dentro de la serie de excavaciones que este Seminario de Arqueología ha llevado a cabo en colaboración con la Dirección del Museo Arqueológico, cabe destacar por la importancia y cantidad de los materiales encontrados la realizada el pasado año 1978 en Tarragona capital. Se trata de la excavación de una cisterna de época romana aparecida con motivo de las obras de construcción de un bloque de viviendas en una zona situada en las cercanías del Foro Romano, entre las calles del Dr. Zamenhoff y prolongación de Capuchinos. La cisterna estaba excavada en la roca natural, aprovechando, en parte, una cavidad de la misma. Sus dimensiones eran 4,6 X 4,20 X 2,40 m., y apareció en parte destruida por la acción de las máquinas excavadoras que la pusieron al descubierto. El suelo de la misma tiene un grosor de 10 cm., aproximadamente, y es de opus testaceum. El revoque de las paredes laterales es de opus signinum, con una capa de aislamiento a base de ceniza y cal. Cabe destacar la ausencia del medio toro característico de las construcciones romanas destinadas a contener líquidos. En sus tres cuartas partes apareció rellena de tierra y escombros. De entre los materiales procedentes de su excavación adelantamos el estudio de los fragmentos escultóricos y del monetario.

Fenología del anillo de crecimiento de Pinus uncinata Ramond y Pinus sylvestris L. en un gradiente altitudinal en los Pirineos Centrales

En el presente trabajo, describimos el desarrollo y la estructura del anillo anual de crecimiento de Pinus uncinata Ramondy Pinus sylvestris L. en un gradiente altitudinal en los Pirineos centrales. Medimos mensualmente el aumento de la anchura del anillo y el número de traqueidas añadidas a lo largo de 1993. En ambas especies, la mayor parte del anillo se forma desde mediados de jimio hasta mediados de julio de 1993. El desarrollo de la madera tardía -formación, coloración y engrasamiento y lignificación de las paredes celulares- comienza en julio y acaba en octubre. El anillo comienza antes su formación en los bosques estudiados de P. sylvestris que en P. uncinata, el cual vive a mayor altitud. P. uncinata forma anillos más estrechos, con menor múmero de células y con mayor heterogeneidad de color de la madera tardía que P. sylvestris. Existe una gran variabilidad entre árboles en la posición de las células de las maderas temprana y tardía a lo largo del anillo de crecimiento. Los distintos patrones fenológicos en el crecimiento del anillo anual, a lo largo del gradiente altitudinal seleccionado, pueden explicarse en parte, por la influencia de distintas condiciones climáticas, principalmente térmicas.

Conservació concertada de flora i de monuments històrics - Comentari

Cerca de Jaca, en las paredes del monasterio de San Juan de la Peña vive un endemismo,Petrocoptis hispanica, que se vio amenazado con motivo de unas obras de restauración que sehicieron hace bastantes años. Entonces, la intervención del instituto Pirenaico de Ecología con el Dr.Montserrat a la cabeza permitieron conservar buena parte de la población, aunque si visitas elmonasterio todavía puede verse la parte de la fachada que fue limpiada.

An AdS/QCD model from tachyon condensation: II

A simple holographic model is presented and analyzed that describes chiral symmetry breaking and the physics of the meson sector in QCD. This is a bottom-up model that incorporates string theory ingredients like tachyon condensation which is expected to be the main manifestation of chiral symmetry breaking in the holographic context. As a model for glue the Kuperstein-Sonnenschein background is used. The structure of the flavor vacuum is analyzed in the quenched approximation. Chiral symmetry breaking is shown at zero temperature. Above the deconfinement transition chiral symmetry is restored. A complete holographic renormalization is performed and the chiral condensate is calculated for different quark masses both at zero and non-zero temperatures. The 0++, 0¿+, 1++, 1¿¿ meson trajectories are analyzed and their masses and decay constants are computed. The asymptotic trajectories are linear. The model has one phenomenological parameter beyond those of QCD that affects the 1++, 0¿+ sectors. Fitting this parameter we obtain very good agreement with data. The model improves in several ways the popular hard-wall and soft wall bottom-up models.