Caracterizació arqueomètrica de les ceràmiques tardanes de la plaça del Rei de Barcelona

Un total de 40 ceràmiques tardanes, en la majoria de casos grolleres, que procedeixen de contextos de la segona meitat del segle VI-segle VII de les excavacions de la plaça del Rei de Barcelona, han estat caracteritzades arqueomètricament mitjançant fluorescència de raigs X (FRX), difracció de raigs X (DRX) i microscòpia òptica de làmina prima (MO). A la mostra estudiada, els resultats han permès establir l"existència de fins a 10 grups diferents, alguns dels quals clarament heterogenis, la qual cosa permet pensar que l"anàlisi d"un nombre més elevat de mostres hauria revelat un nombre encara més gran de produccions en el jaciment. Entre les produccions caracteritzades se n"ha identificat una de ceràmica comuna fina de producció local o regional, així com nou de ceràmiques grolleres tant importades com locals i/o regionals.

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.

Goya's artwork imaging with Terahertz waves

In this paper we use a Terahertz (THz) time-domain system to image and analyze the structure of an artwork attributed to the Spanish artist Goya painted in 1771. The THz images show features that cannot be seen with optical inspection and complement data obtained with X-ray imaging that provide evidence of its authenticity, which is validated by other independent studies. For instance, a feature with a strong resemblance with one of Goya"s known signatures is seen in the THz images. In particular, this paper demonstrates the potential of THz imaging as a complementary technique along with X-ray for the verification and authentication of artwork pieces through the detection of features that remain hidden to optical inspection.

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.

Anàlisi arqueològica de tres alambins procedents del quarter de Sant Pere de Barcelona

Durant les excavacions de l"avinguda de Cambó dutes a terme el 1986 es van recuperar, entre d"altres, diversos elements identificats com a alambins, que han estat relacionats amb la tècnica d"aplicació d"or al foc sobre objectes metàl·lics, activitat que podria haver tingut lloc en un dels àmbits identificats en el quarter de Sant Pere en època medieval.Amb l"objectiu de comprovar si els alambins recuperats són, d"una banda, de producció local i, d"una altra, si presenten evidències que puguin corroborar el seu ús en aquesta tècnica, es va procedir a la caracterització arqueomètrica de tres d"aquests objectes (BCN224, BCN225 i BCN226), de manera que la seva composicióquímica s"ha determinat per fluorescència de raigs X (FRX) i la composició mineralògica a través de la difracció de raigs X (DRX). Per a l"estudi de la microestructura i estadi de sinterització de la matriu i del vidriat, s"han dut a terme observacions i microanàlisis per microscòpia electrònica de rastreig (MER) utilitzant un microscopi Jeol JSM-840 equipat amb un detector de dispersió d"energies de raigs X (EDX). A més, amb la finalitat de fixarles característiques macroscòpiques dels individus es van realitzar observacions a partir de fractures fresques emprant una lupa binocular Olympus SZX10, amb una font d"il·luminació de llum freda Olympus KL 1500 LCD equipada amb filtre de llum de dia i una càmera digital de microfotografia Olympus DP25, amb el software Cell"A. La lupa binocular està equipada amb un objectiu de 1X i oculars de 10X, amb un zoom continuat, amb posicions fixes, que permet fer observacions de 6.3X a 63X, però que s"han estandarditzat a 10X i 25X.

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.

El taller ceràmic d'època romana del carrer Princesa de Barcelona. Estudi arqueològic de les restes i estudi arqueomètric del material ceràmic

Les excavacions arqueològiques recents realitzades al carrer Princesa 21 de Barcelona han tret a la llum noves evidències de la producció de ceràmica romana a l"àrea perifèrica de Barcino. Aquest taller ceràmic presenta dues fases cronològiques, des del començament del segle I dC fins al II dC, i va produir àmfores Pascual 1 i Dressel 2-4, ceràmica comuna, tegulae i pondii. L"origen d"aquest taller està relacionat amb la fundació de la colònia romana de Barcino i la imposició de les estructures econòmiques i socials romanes. Fins avui, s"han caracteritzat 42 fragments d"àmfores Pascual 1, 2 pondii i 4 mostres d"argila mitjançant la tècnica de Fluorescència de Raigs X (FRX) en l"estudi de procedència, i les composicions mineralògiques s"han determinat mitjançant anàlisis per Difracció de Raigs X (DRX) per entendre"n les característiques tecnològiques. Aquestes anàlisis demostren una producció amfòrica homogènia i estandarditzada, realitzada amb una pasta calcària normalment cuita a alta temperatura.

On the multiwavelength spectrum of the microquasar 1E1740.7-2942

The microquasar 1E 1740.7-2942 is a source located in the direction of the Galactic Center. It has been detected at X-rays, soft gamma-rays, and in the radio band, showing an extended radio component in the form of a double-sided jet. Although no optical counterpart has been found so far for 1E 1740.7-2942, its X-ray activity strongly points to a galactic nature. Aims.We aim to improve our understanding of the hard X-ray and gamma-ray production in the system, exploring whether the jet can emit significantly at high energies under the light of the present knowledge. Methods.We have modeled the source emission, from radio to gamma-rays, with a cold-matter dominated jet model. INTEGRAL data combined with radio and RXTE data, as well as EGRET and HESS upper-limits, are used to compare the computed and the observed spectra. Results.From our modeling, we find out that jet emission cannot explain the high fluxes observed at hard X-rays without violating at the same time the constraints from the radio data, favoring the corona origin of the hard X-rays. Also, 1E 1740.7-2942 might be detected by GLAST or AGILE at GeV energies, and by HESS and HESS-II beyond 100 GeV, with the spectral shape likely affected by photon-photon absorption in the disk and corona photon fields.

Discovery of a High-Energy Gamma-Ray-Emitting Persistent Microquasar

Microquasars are stellar x-ray binaries that behave as a scaled down version of extragalactic quasars. The star LS 5039 is a new microquasar system with apparent persistent ejection of relativistic plasma at a 3 kiloparsec distance from the sun. It may also be associated with a gamma-ray source discovered by the Energetic Gamma Ray Experiment Telescope (EGRET) on board the COMPTON-Gamma Ray Observatory satellite. Before the discovery of LS 5039, merely a handful of microquasars had been identified in the Galaxy, and none of them was detected in high-energy gamma-rays.

Studying the non-thermal lobes of IRAS 16547-4247 through a multi-wavelength approach

In recent years, massive protostars have turned out to be a possible population of high-energy emitters. Among the best candidates is IRAS 16547-4247, a protostar that presents a powerful outflow with clear signatures of interaction with its environment. This source has been revealed to be a potential high-energy source because it displays non-thermal radio emission of synchrotron origin, which is evidence of relativistic particles. To improve our understanding of IRAS 16547-4247 as a high-energy source, we analyzed XMM-Newton archival data and found that IRAS 16547-4247 is a hard X-ray source. We discuss these results in the context of a refined one-zone model and previous radio observations. From our study we find that it may be difficult to explain the X-ray emission as non-thermal radiation coming from the interaction region, but it might be produced by thermal Bremsstrahlung (plus photo-electric absorption) by a fast shock at the jet end. In the high-energy range, the source might be detectable by the present generation of Cherenkov telescopes, and may eventually be detected by Fermi in the GeV range.

A microquasar model applied to unidentified gamma-ray sources

Among unidentified gamma-ray sources in the galactic plane, there are some that present significant variability and have been proposed to be high-mass microquasars. To deepen the study of the possible association between variable low galactic latitude gamma-ray sources and microquasars, we have applied a leptonic jet model based on the microquasar scenario that reproduces the gamma-ray spectrum of three unidentified gamma-ray sources, 3EG J1735-1500, 3EG J1828+0142 and GRO J1411-64, and is consistent with the observational constraints at lower energies. We conclude that if these sources were generated by microquasars, the particle acceleration processes could not be as efficient as in other objects of this type that present harder gamma-ray spectra. Moreover, the dominant mechanism of high-energy emission should be synchrotron self-Compton (SSC) scattering, and the radio jets may only be observed at low frequencies. For each particular case, further predictions of jet physical conditions and variability generation mechanisms have been made in the context of the model. Although there might be other candidates able to explain the emission coming from these sources, microquasars cannot be excluded as counterparts. Observations performed by the next generation of gamma-ray instruments, like GLAST, are required to test the proposed model.

LS 5039: A runaway microquasar ejected from the galactic plane

We have compiled optical and radio astrometric data of the microquasar LS 5039 and derived its proper motion. This, together with the distance and radial velocity of the system, allows us to state that this source is escaping from its own regional standard of rest, with a total systemic velocity of about 150 km/s and a component perpendicular to the galactic plane larger than 100 km/s. This is probably the result of an acceleration obtained during the supernova event that created the compact object in this binary system. We have computed the trajectory of LS 5039 in the past, and searched for OB associations and supernova remnants in its path. In particular, we have studied the possible association between LS 5039 and the supernova remnant G016.8-01.1, which, despite our efforts, remains dubious. We have also discovered and studied an HI cavity in the ISM, which could have been created by the stellar wind of LS 5039 or by the progenitor of the compact object in the system. Finally, in the symmetric supernova explosion scenario, we estimate that at least 17 solar masses were lost in order to produce the high eccentricity observed. Such a mass loss could also explain the observed runaway velocity of the microquasar.

Domain matched epitaxial growth of Bi1.5Zn1Nb1.5O7 thin films by pulsed laser deposition

Bi1.5Zn1Nb1.5O7 (BZN) epitaxial thin films were grown by pulsed laser deposition on Al2O3 with a double ZnO buffer layer through domain matching epitaxy (DME) mechanism. The pole figure analysis and reciprocal space mapping revealed the single crystalline nature of the thin film. The pole figure analysis also shows a 60º twinning for the (222) oriented crystals. Sharp intense spots in the SAED pattern also indicate the high crystalline nature of BZN thin film. The Fourier filtered HRTEM images of the BZN-ZnO interface confirms the domain matched epitaxy of BZN with ZnO buffer. An electric field dependent dielectric tunability of 68% was obtained for the BZN thin films with inter digital capacitors patterned over the film.

Les pintures murals de la basílica paleocristiana de «Es Cap des Port» (Fornells, Menorca): materials i tècniques

[cat]El present treball ofereix una revisió de les pintures murals de la basílica de «Es Cap des Port» (Fornells, Menorca), així com un estudi de caracterització arqueomètrica deIs materials i tècniques per microscòpia òptica, tant amb lupa binocular com amb microscopi petrogràfic mitjançant làmina prima, difracció de raigs X i microscòpia electrònica de rastreig. Els resultats han permès identificar els pigments emprats, així com la seva tècnica d'aplicació. Igualment, han permès caracteritzar els morters i han desvelat l' existència de dos tipus diferents de suport. Malgrat aquestes diferències en els morters, els pigments són sempre els mateixos per a tots els conjunts pictòrics caracteritzats [eng] The present paper offers a revision of the wall paintings found at the early Christian church of 'Es Cap des Port' (Fornells, Menorca). Moreover, the materials and techniques employed have been archaeometrically studied by means of optical microscopy, both with steromicroscope and petrographic microscope by thin section, X-ray diffraction and scanning electron microscopy. The results enable to identify the pigments used, as well as the techniques of application. It has also been possible to characterize the mortars, revealing the existence of two different types of support. In spite of these differences in the mortars, the pigments used are the same ones for all the studied wall paintings

EVN+MERLIN observations of microquasar candidates at low galactic latitudes

In an attempt to increase the number of known microquasars, Paredes et al. (2002) have presented a long-term project focused on the search for new objects of this type. They performed a cross-identification between X-ray and radio catalogs under very restrictive selection criteria for sources with |b|<5 degrees, and obtained a sample of 13 radio-emitting X-ray sources. Follow-up observations of 6 of these sources with the VLA provided accurate coordinates, which were used to discover optical counterparts for all of them. We have observed these six sources with the EVN and MERLIN at 5 GHz. Five of the six objects have been detected and imaged, presenting different morphologies: one source has a two-sided jet, three sources have one-sided jets, and one source is compact. With all the presently available information, we conclude that two of the sources are promising microquasar candidates in our Galaxy.